Abstracts received

Invited talks

1 - Machine Learning in Meteor Science: Advances and Applications

Science Topic(s): Future Methods and Techniques

Simon Anghel [early-career researcher] (LTE - Observatoire de Paris)

Machine learning (ML) has emerged as a transformative tool in all data science. This talk explores how ML is revolutionizing meteoroid science, offering new insights into detection systems, filtering methods, origin and compositional studies while paving the way for future interdisciplinary applications.

2 - Missing Pieces: The Atmospheric Filter and the Curious Case of Carbonaceous Chondrites

Science Topic(s): Meteoroid Sources, Dynamical Evolution

Patrick Shober [early-career researcher] (NASA)
co-authors: Hadrien Devillepoix, Jeremie Vaubaillon, Simon Anghel, Sophie Deam, Eleanor Sansom, Francois Colas, Brigitte Zanda, Pierre Vernazza, Phil Bland

Multiple attempts have been made to identify robust orbital connections between meteorites and near-Earth asteroids, yet recent statistical tests show no convincing excess of shared orbits among recovered falls and known NEAs. Meanwhile, carbonaceous chondrites—especially CI and CM types—often exhibit short cosmic-ray exposure (CRE) ages, at times only a few thousand to a few hundred thousand years (Shober et al. 2024), implying a recent ejection in near-Earth space is possible. Also, despite models predicting that over half of Earth-impacting meteoroids should be carbonaceous (Broz et al. 2024), these meteorites remain notably underrepresented in worldwide collections (~4%). To reconcile these observations, we combined meteoroid stream modeling with an analysis of how Earth’s atmosphere modifies the meteorite population. Drawing on nearly 8,000 fireball detections and 500 potential meteorite-dropping events from 19 networks across 39 countries, we explored which orbits produce more durable fragments and which yield relatively few recoverable meteorites. Our findings indicate that “perihelion filtering”—driven by thermal fracturing near the Sun—removes fragile meteoroids long before atmospheric entry. Consequently, the hallmark short CRE ages of carbonaceous chondrites and the near absence of carbonaceous streams at near-Earth distances are likely intertwined results of this intense pre-impact selection and rapid orbital decoherence of minor streams (Shober et al. 2025a,b).

3 - Advances in Meteor Spectroscopy: Observational and Laboratory Perspectives

Science Topic(s): Meteor Physics and Chemistry

Adriana Pisarčíková [early-career researcher] (Astronomical Institute of the Czech Academy of Sciences)
co-authors: Jiří Borovička, Pavol Matlovič

Meteor spectroscopy has become a key method for determining the composition of meteoroids entering Earth’s atmosphere. This talk will review the current state of meteor spectroscopy, focusing on both observational techniques and recent advances in laboratory simulations. Current methods rely on meteor emission spectra obtained using photographic and video spectrographs. In low-resolution spectra, relative line intensity ratios of Na I-1, Mg I-2, and Fe I-15 are used to determine spectral type. High-resolution spectra enable the application of radiative transfer model to estimate elemental abundances more accurately. Nonetheless, unambiguously associating observed spectral characteristics with particular meteoroid materials is still challenging. Recently, a large and diverse set of high-resolution meteorite ablation spectra was obtained under atmospheric entry-like conditions using plasma wind tunnel experiments at the Institute of Space Systems, University of Stuttgart. The results show the potential of line intensity variations-based classification for improved compositional determination of asteroidal meteoroids, though limitations may exist in distinguishing meteorite types with similar compositions, such as different classes of ordinary chondrites. To address this, we applied a comprehensive radiative transfer model (accounting for thermal equilibrium and self-absorption) to laboratory meteorite ablated spectra for a more accurate evaluation of meteoroid composition.

4 - The ESA’s LUMIO mission: A new window into meteoroid characterization through far side lunar impact flash observations

Science Topic(s): Impacts on Other Planets/Surfaces

Eloy Peña Asensio [early-career researcher] (Politecnico Milano)

The ESA’s Lunar Meteoroid Impact Observer (LUMIO) is a 12U CubeSat designed to detect Lunar Impact Flashes (LIFs) on the Moon’s far side from a quasi-halo orbit around Earth-Moon L2. Led by Politecnico di Milano with support from several space agencies, LUMIO will provide the first continuous monitoring of the lunar hemisphere hidden from Earth. LUMIO will detect LIFs in the 450–950 nm range from impacts >10⁻⁶ kt (>1 g), enabling new constraints on the meteoroid flux in cislunar space. The Science Team is developing methods to classify LIFs as sporadic or stream-related based on spatial and temporal patterns. However, due to the absence of velocity data, we emphasize the need for coordinated ground-based meteor observations during LUMIO’s one-year mission starting in 2028. Simultaneous meteor shower monitoring will aid in associating LIFs with streams and inferring impactor properties through size-frequency extrapolation. LUMIO’s timing and location data will support follow-up crater searches by LRO, helping calibrate energy–crater size laws. Dual-band detections will allow flash temperature estimation and investigation of thermodynamics–morphology links. We call for community participation in a coordinated LIF observation campaign and support through meteoroid stream modeling to enhance source attribution and reconstruct stream structures.

Contributed talks

10 - Annual variation of sodium in the Geminids spectra over 6-years

Science Topic(s): Composition and Physical Properties

Shinsuke Abe (Nihon University, Japan)
co-authors: Keita Kikuchi, Takashi Sekiguchi, Koji Maeda, Tomoko Arai

We present statistical results of Na emission using over 1000 Geminids meteoroids spectra over multiple years from 2017 to 2022. The goal is to characterize long-term variations in Na line intensities and understand the effects of meteor size, solar longitude, and composition ratio (Na/Mg/Fe) on Na depletion. Using consistent annual spectral observations, we measured the relative intensities of Na, Mg, and Fe emission lines and examined trends over time. We found that the Na/Mg and Na/Fe intensity ratios varied significantly from year to year. Na intensity was found to be correlated with meteoroids size and solar longitude. These results have important implications for the evolution of the dust stream of asteroid 3200 Phaethon and indicate that Na volatilization and compositional gradients are ongoing in the Geminid meteorite stream.

11 - Enhancing Meteoroid Research Through the NASA Science Explorer (SciX)

Science Topic(s): Future Methods and Techniques

Simon Anghel [early-career researcher] (LTE - Paris Observatory)

This presentation introduces the NASA Science Explorer (SciX), a comprehensive digital library platform that represents a transformative approach to research. As meteoroid studies increasingly span multiple disciplines—from cosmic dust dynamics to planetary defense—researchers face challenges in efficiently discovering and integrating knowledge across traditional domain boundaries. SciX addresses this need by unifying research literature, data, and software from astronomy, planetary science, heliophysics, and earth science within a single discovery environment. Built on the foundation of the Astrophysics Data System (ADS) but significantly expanded, SciX offers meteoroid researchers access to over 25 million bibliographic records with advanced search capabilities specifically valuable for interdisciplinary questions. This presentation will demonstrate how SciX can be leveraged to enhance meteoroid research workflows through practical examples and use cases.

12 - Using the lunar impact record to decipher the flux of kilometric asteroids on Earth

Science Topic(s): Meteoroid Sources, Influx of Interplanetary and Interstellar Material

Lagain Anthony (CEREGE, Aix-Marseille Université / Curtin University)
co-authors: Miroslav. Brož, John Fairweather, Pierre Vernazza, Yoann Quesnel, Alexis Licht, Alessandro Morbidelli, Konstantinos Servis, Anthony Ozerov, Phil Bland, Gretchen Benedix

Asteroid breakups in the main belt between Mars and Jupiter have driven the flux of impactors to the inner Solar System for at least three billion years. However, no clear evidence of variations in impact rates over that time has been found in the geological record of terrestrial bodies. Here, we use a neural network to detect over one million lunar craters larger than ~100 m and determine the ages of 211 craters exceeding 20 km in diameter. Our results reveal a prolonged period of intense bombardment between 1.4 and 0.9 billion years ago, during which the formation rate of 20–40 km lunar craters increased by a factor of 3.8 ± 0.2. To trace the origin of this surge, we perform dynamical simulations that reconstruct the past flux of impactors. We identify the Flora asteroid family as the primary source. On Earth, this translates to approximately 1,600 impact events by objects larger than 1 km during the Proterozoic, occurring roughly every 255,000 years. This impact frequency is comparable to the estimated biological recovery time following the Chicxulub event (200,000–300,000 years), which amplified the Cretaceous mass extinction. The end of this prolonged bombardment coincides with the emergence of multiple eukaryotic clades, suggesting that asteroid impacts may have influenced the evolution of complex life.

13 - Reassessing 1200 meteor showers and their links to the near-Earth environment

Science Topic(s): Meteoroid Sources

Aishabibi Ashimbekova [early-career researcher] (Observatoire de Paris, PSL)
co-authors: Jeremie Vaubaillon

The International Astronomical Union (IAU) currently lists around 1200 meteor showers, raising questions about their reality given our current understanding of the Solar System, and the need for a comprehensive re-evaluation. This ongoing study aims to assess the feasibility of these showers originating from known near-Earth comets and asteroids, considering their orbital dynamics, dust production capabilities and residence times. Our study focuses on several key aspects: 1. Impact Configurations from Near-Earth Comets: We estimate the number of possible meteor shower orbits produced by near-Earth comets, taking into account the Kozai and precession cycles. 2. Active Asteroids as Parent Bodies: We examine active asteroids as potential sources of meteor showers, considering their quantity, dust production rates and lifetime expectancies. 3. Near-Earth Asteroids Contribution: We explore the role of near-Earth asteroids in generating meteor showers. By integrating these factors, we aim to determine if the current near-Earth environment can indeed support the existence of 1200 meteor showers. This work-in-progress seeks to align our understanding of meteor shower origins with the observed data. The findings will contribute to our broader comprehension of the dynamics and interactions within the near-Earth environment.

14 - Physical properties of kappa Cygnid and eta Virginid meteoroids

Science Topic(s): Composition and Physical Properties

Jiri Borovicka (Astronomical Institute of the Czech Academy of Sciences)
co-authors: Pavel Spurny

Meteor showers kappa Cygnids (12 KCG) and eta Virginids (11 EVI) are established showers with some common characteristics. Both exhibit low-level activity lasting for about two weeks and are rich in fireballs. In both cases, the activity is periodic and is probably mostly caused by meteoroids in mean motion resonances with Jupiter. Kappa Cygnids are in the 5:3 resonance with the period of ~ 7 years; eta Virginids are in the 3:1 resonance with the period ~ 4 years. In all these aspects, both showers are similar to the Taurid branch, which is in the 7:2 resonance. The physical appearance of fireballs is, however, different. While kappa Cygnids are known for their bright flares and are obviously very fragile, eta Virginids behave more like asteroidal meteors. In this work, we use the data from the European Fireball Network, in particular detailed radiometric light curves, to model atmospheric fragmentation of individual meteoroids of various masses and to infer their physical properties such as density, strength, and internal structure. The results are compared with Taurids studied earlier by us with the same method. Given the absence of knowledge regarding the parent body of either the kappa Cygnids or the eta Virginids, the nature of their parent bodies will be discussed.

15 - A Search for Hydroacoustic Signals from Bolides

Science Topic(s): Large impacts and Planetary Defence, Future Methods and Techniques

Peter Brown (University of Western Ontario)
co-authors: Luke McFadden, Denis Vida

Acoustic signals from bolides have been detected directly on microbarometers (as infrasound) and on seismographs via seismo-acoustic coupling of acoustic waves to the solid Earth. However, to date, there has not been a confirmed instance where a hydroacoustic coupled wave has been detected in the ocean by a hydrophone. Theoretical studies suggest that an airborne explosive source will couple less than 0.0001% of its energy into the ocean. Complicating fireball hydroacoustic detection is the requirement that signals be trapped in the Sound Fixing and Ranging (SOFAR) channel, some 1.5 km below the surface, to be detectable by distant hydrophone stations. Here we present a search for hydroacoustic signals associated with fireballs having multi-kiloton and larger energies as reported by US Government Sensors. We use data recorded by the hydrophone network of the International Monitoring System operated by the Comprehensive Test Ban Treaty Organization. Using the expected signal arrival and backazimuth we isolate probable fireball-produced hydroacoustic signals. Our survey finds that underwater reflections and T-phase arrivals associated with Earthquakes complicate signal association, but we find several bolides produce likely signals. We present the evidence for the fireball hydroacoustic signal association for the most convincing cases and estimate the hydroacoustic coupling efficiency of airwaves produced by large bolides from these measurements.

16 - New Zealand’s first camera-assisted meteorite recovery

Science Topic(s): Meteorite Recoveries

Daniel Burgin [student] (Space Science and Technology Centre, Curtin University, Australia; Fireballs Aotearoa, New Zealand)
co-authors: Thomas W. C. Stevenson, James M. Scott, Marshall C. Palmer, Denis Vida, Dennis Behan, Mia R. Boothroyd, David Grieg, Peter McKellar, Terry Richardson, Jim Rowe, Damir Šegon, Jesse Stayte, Tingting Wang, Jack Weterings, Steve Wyn-Harris

At 9:04 pm local time on 13 March 2024, a large fireball was seen over the central South Island of New Zealand. The fireball was captured on five Raspberry Pi Meteor Station (RMS) cameras and one Allsky7 camera included in New Zealand’s meteor camera network, Fireballs Aotearoa. The trajectory, velocity, and origin of the fireball were calculated using data from RMS cameras. Skyfit2 modelling indicated the fireball lasted 6.72 s, descending from 96 to 23.3 km elevation and decelerating from 18 to 5 km/s. The rock originated from an Aten-type orbit. A dark flight solution indicated the rock landed within a former braided river channel of the Takapō River on public conservation land. A public search organised by Fireballs Aotearoa was undertaken on 20 March 2024. Remarkably, the meteorite was found within 30 minutes of the search initiation, partially embedded in a small crater within the local flood-plain greywacke gravels. Subsequent analysis has identified the 810 g Takapō meteorite as an L5 chondrite. This is the first instrumentally-observed meteorite fall in New Zealand, and demonstrates the ability of Fireballs Aotearoa to track and recover meteorites.

17 - Correcting meteor radar observing biases with simultaneous optical observations

Science Topic(s): Influx of Interplanetary and Interstellar Material

Margaret Campbell-Brown (University of Western Ontario)

Radar observations of meteors can provide fluxes for showers and outbursts 24 hours a day. These fluxes suffer from observing biases, like initial trail radius. A new study of more than 10,000 simultaneous faint optical and radar meteors has been used to look at radar observing biases. The optical meteors were captured with four very sensitive EMCCD video cameras observing in two pairs, so that orbits could be calculated for each. Meteors which fulfilled the specular condition for the radar at some point along their trajectory were pulled from the radar data at the Canadian Meteor Orbit Radar’s three frequencies (17.45, 29.85 and 38.15 MHz). Sorted by speed, the data show that all three frequencies miss meteors at very low speeds, likely due to a lack of ionization at low collision energies. As expected, the highest frequency radar misses the highest fraction of fast meteors, though the height ceiling does not behave as expected. A new correction factor for each frequency has been calculated, which is similar to the initial radius correction calculated using simultaneous radar echoes at different frequencies.

18 - Exploring a New Approach to Simulating Meteors: Going Beyond DSMC

Science Topic(s): Meteor Physics and Chemistry, Future Methods and Techniques

Dakota Cecil [student] (Western University)
co-authors: Margaret Campbell-Brown

In an effort to better constrain meteoric luminous efficiencies (tau) of small mm-sized meteoroids, an attempt to fully numerically simulate meteor entry was conducted. As is typical with low density simulations (e.g., Bariselli et al., 2018), the Direct Simulation Monte Carlo (DSMC) method was used to simulate a few 1 mm meteoroids at various altitudes. This process was preliminary, and served to determine the viability of simulating meteors with DMSC. It was found that the high speeds and large differences in densities of meteoric elements made the off-the-shelf DSMC implementation (SPARTA) too computationally expensive for accurate luminous efficiency calculations. To overcome the statistically limited nature of DSMC, a new deterministic method is being sought, with the leading candidate being the Fast Spectral Method (FSM). This method represents the velocity distribution of air and ablated meteoroid particles spectrally, via a Fourier Series. This allows low density meteoric species to be properly represented, a necessity for accurately determining tau. As no off-the-shelf FSM solver currently exists, efforts have been focused on developing a highly optimized implementation. Unfortunately, the FSM suffers a similar computational scaling penalty as the DSMC method with increasing meteor speed. A new wavelet-based method is currently being developed to address this problem.

19 - MOFID : The Moroccan Meteor Detection Network

Science Topic(s): Meteor Physics and Chemistry, Meteorite Recoveries

Hasnaa Chennaoui Aoudjehane (Hassan II University of Casablanca, Faculty of Science Ain Chock)
co-authors: Hasnaa1 Chennaoui Aoudjehane1, Hadrien2 Devillepoix2, Zouhair3 Benkhaldoun3, Hassan4 Darhmaoui4

MOFID (Moroccan Observatory for Fireball Detections) is an all-sky camera network established in Morocco since 2015 through a partnership between the University of Perth and Hassan II University of Casablanca. Morocco, among the world's richest countries in meteorite finds and observed falls [1], inspired its creation. MOFID is part of the Desert Fireball Network (DFN), now the Global Fireball Network (GFN) [2], and is managed by the ATTARIK Foundation. Developed in collaboration with Oukaimeden Observatory (Cadi Ayyad University), MOFID involves partners such as Al Akhawayn University, Moroccan schools, and private supporters. The network consists of ten cameras, though only a few remain installed at Oukaimeden, Al Akhawayn, and a school in Ouzoud. Cameras were previously placed in Agoudal and Aït Ben Haddou. MOFID successfully detected numerous meteors, calculating their trajectories and fall zones. On August 6, 2021, a meteor observed by MOFID and Spanish networks enabled precise fall location calculation in the Rif region and a potential parent asteroid identification [3]. The Taghzout meteorite was later recovered and classified [4]. Despite technical challenges, MOFID has contributed significantly to planetary science in Morocco, fostering national and international collaborations and engaging students in research. The recent expansion through the FRIPON [5] and GMN [6] networks will further enhance meteor detection and research.

20 - Dynamical and Physical Properties of Decameter-size Earth Impactors

Science Topic(s): Composition and Physical Properties, Large impacts and Planetary Defence

Ian Chow [student] (University of Western Ontario)
co-authors: Peter G. Brown

Numerous decameter-size asteroids have been observed impacting Earth, often appearing as spectacular fireballs in the atmosphere. These objects can have kinetic energies equivalent to hundreds of kilotons of TNT, posing a hazard if they impact populated areas. In 2022, the US Space Force publicly released decades of previously classified fireball data from US Government (USG) satellite sensors, the most comprehensive dataset of meter-size and larger fireballs to date. From USG sensor data, we estimate a decameter-size impact occurs every ~2-3 years, an impact rate consistent with previous fireball and acoustic estimates. In contrast, several independent recent near-Earth object (NEO) models based on telescopic surveys predict such objects to impact Earth once every ~20-40 years, an order-of-magnitude difference. The cause of this "decameter gap" remains unclear. Using this newly available USG sensor data, we present the first population-level study characterizing the dynamical and physical properties of decameter-size impactors. We analyze the dynamical origins of decameter-size impactors and NEOs and assess several possible explanations for the "decameter gap." We also introduce a novel Bayesian inference method for modelling their atmospheric ablation based on dynamic nested sampling and apply it to characterize uncertainties in the physical properties of these objects for the first time.

21 - Seismo-acoustic signals of fireballs: Comparing different types of atmospheric entry events.

Science Topic(s): Composition and Physical Properties, Meteoroid Impact Physics

Iona Clemente (Curtin University)
co-authors: Eleanor K. Sansom, Hadrien A. R. Devillepoix, Taichi Kawamura, Benjamin A. Fernando, Raphael F. Garcia, Olivia Collet

Re-entry objects, particularly sample return capsules (SRCs) like the one from the Hayabusa2 mission, are of great interest to the meteor science community. Their similarity to slow meteors during atmospheric entry, along with the advantage of knowing their entry time and location, makes them valuable for research. It is well established that large enough meteoroid entries (exceeding 10 cm diameter) generate shockwaves (Bronshten et al., 1965; ReVelle et al., 1976, 2008; Silber et al., 2018). These shockwaves originate from the atmospheric hypersonic passage or fragmentation events (Ceplecha et al., 1998; ReVelle, 1976), which occur when the ram pressure exceeds the meteoroid’s cohesive strength (Cevolani, 1994, Stevanovic et al., 2017). SRCs, designed to withstand atmospheric re-entry, do not typically fragment. Consequently, the shockwave generated during these re-entries is likely to originate from the hypersonic entry, commonly referred to as the ballistic shock. In this study, we analyse seismic signals from the Hayabusa2 SRC re-entry on December 5th, 2020, over the Woomera Prohibited Area in South Australia. The event was recorded by a dense network of seismic stations (Eakin, 2018; O’Donnell et al., 2020), offering a unique opportunity to examine waveform, signal polarization and conduct cross-correlation analyses. We also compare seismic signatures from the Hayabusa2 SRC re-entry to other re-entry and natural fireball events, discussing similarities and differences.

22 - The Southern Hemisphere Asteroid Research Consortium (SHARC)

Science Topic(s): Composition and Physical Properties, Large impacts and Planetary Defence

David Coward (University of Western Australia)
co-authors: ED Kruzins, Edwin Peters, Shinji Horiuchi, John Kennewell, Arie Verveer, Hadrien Devillepoix, Ellie Samson, Guifre Molleracalves, Evan Dilley, Dorota Mieczkowska

The Southern Hemisphere Asteroid Research Consortium (SHARC) is a research intensive and informal entity comprised of UNSW (Canberra), UTas, UWA and Curtin University. The research focus of SHARC is characterising potentially hazardous Earth orbit crossing asteroids, the so-called Apollo and Aten types. In addition to the Australian universities, SHARC is enabled by participation of federal agencies, the Commonwealth Scientific and Industrial Research Organisation (CSIRO) and the NASA Jet Propulsion Laboratory (JPL). Several Australian SHARC members are also International Asteroid Warning Network (IAWN) delegates, contributing astrometric and photometric data on select near Earth asteroid close approaches. As the next generation of asteroid surveying instruments comes online over the next few years (Rubin, NEO Surveyor etc.), the distinction between asteroids and meteoroids is beginning to blur, offering unique opportunities to study the small asteroid population.This presentation will summarise the main activities of SHARC and outline a roadmap for the future.

23 - UKFAll rising – the expansion of the UK Fireball Alliance.

Science Topic(s): Influx of Interplanetary and Interstellar Material, Meteorite Recoveries

Luke Daly (School of Geographical and Earth Sciences, University of Glasgow)
co-authors: Luke Daly, Andrew Smedley, Ashley King, Katherine Joy, Gareth Collins, Jim Rowe, Charlotte Bays, Peter Campbell-Burns, Apostolos Christou, Natasa Vasiliki Almedia, Will Gater, Jana Horák, Mark McIntyre, Sarah McMullan, Chloe Kadir, Áine O’Brien

The UK Fireball Alliance (UKFAll) was established in 2018 to bring together the UK’s academic and citizen science led meteor camera networks as well as meteorite curators and researchers to image fireballs and recover meteorites in the UK. Part of this collaboration involved developing and deploying a code to rapidly translate meteor data outputs from diverse hardware and software into a universal standard [1,2]. In 2021 UKFAll was instrumental in recovering the Winchcombe meteorite, a rare CM-type carbonaceous chondrite and the first UK meteorite fall recovered for 30 years [3]. This success led to a rapid expansion of citizen science led UK Meteor Network, Global Meteor Network, NEMETODE network and All Sky 7 network. In addition, UKFAll received UKRI STFC grants to improve curation of UK meteorite collections (ST/V000799/1) and maintain existing cameras and purchase additional cameras for academic led SCAMP and UKFN networks (ST/Y004817/1), almost doubling the size of these networks to ~40 sites to achieve complete coverage of the night skies across the UK. Here we will outline the expansion and current capabilities of UKFAll and lessons learned from recent fireball observations and associated search expeditions. [1] Rowe, J., et al., (2020) EPSC, 2020-856. [2] Daly, L., et al., (2020) EPSC, 2020-705. [3] King, A. J., et al., (2022) Science Advances, 8(46), eabq3925.

24 - A Near-Earth Object Model Calibrated to Earth Impactors

Science Topic(s): Meteoroid Sources, Dynamical Evolution

Sophie E. Deam [student] (Space Science and Technology Center, Curtin University, Australia)
co-authors: Hadrien Devillepoix, David Nesvorny

Near-Earth object (NEO) models are a useful tool for interpreting asteroid behaviour in near-Earth space (perihelion distances < 1.3 au). They can predict many asteroid properties such the size-dependent transport from the main-belt (Granvik et al., 2018; Nesvorný et al., 2023) the disruptive processes of low perihelia passage (Granvik et al., 2016; Wiegart et al., 2020) the frequency of Earth impactors (Harris & Chodas, 2021; Morbidelli et al., 2020) and trace the origins of meteorites to the main asteroid belt (e.g. Brown et al., 2023). We approach NEO modelling from a new direction and calibrate a NEO model to Earth impactors with data from the Global Fireball Observatory (Devillepoix et al., 2020), using more than 1,200 triangulated fireballs to probe the centimetre to metre-sized bodies. I will present the modelling methodology and first results. Brown, P. G. et al. 2023 MAPS 58 1773. Devillepoix, H. A. R. et al. 2020 P&SS 191 105036. Granvik, M. et al. 2016 Nat. 530 303. Granvik, M. et al. 2018 Icarus 312 181. Harris, A. W. & Chodas, P. W. 2021 Icarus 365 114452. Morbidelli, A. et al. 2020 Icarus 340 113631. Nesvorný, D. et al. 2023 AJ 166 55. Wiegert, P. et al. 2020 AJ 159 143.

25 - Real-time Drone-Assisted Meteorite Recovery: Towards Full Operational Capability

Science Topic(s): Meteorite Recoveries, Future Methods and Techniques

Hadrien Devillepoix [early-career researcher] (Curtin University)
co-authors: Lewis Lakerink, Seamus Anderson, Nancy Tippaya

We present an automated drone survey system designed for rapid and accurate meteorite identification in a remote field setting. The system employs high-resolution drone imagery, which is transmitted in real-time to the cloud via satellite communications. The images are processed using state of the art object detection machine learning algorithms to pinpoint potential meteorites. A user-friendly web interface allows users to review and refine the candidates, taking advantage of crowdsourcing for this task. Finally, precise coordinates are generated to guide field teams for efficient follow-up, down to sub-metre precision thanks to Real Time Kinematics-enabled GPS. This integrated workflow significantly reduces meteorite search time. Although it was developed for the specific use case of meteorites, this process can translate to a wide range of applications. We are currently looking for partners to trial this technology in different terrains.

26 - Spectroscopic Observations of Tracked mm-sized Meteors

Science Topic(s): Composition and Physical Properties, Meteor Physics and Chemistry

Logan Dewsnap [student] (University of Western Ontario)
co-authors: Margaret Campbell-Brown

The Canadian Automated Meteor Observatory (CAMO) system tracks meteors in real time, and allows high-resolution, high-framerate observations to a precision of order 1 m. Recently, this system has been augmented with a spectral camera, sensitive to a range of approximately 400-900nm, providing spectra for meteors tracked by the main system. In this work we will present results from meteors whose spectra were well-observed. We examine the strengths of various contributing emissions lines, including relative scaling versus meteor speed, height, and the initial mass (determined from dynamical modelling with the main CAMO cameras). We additionally consider the effect of such scaling on observed luminous efficiency for non-spectral cameras of different passbands. For a subset of the meteors, where useful per-frame spectra are available over a significant portion of the meteor's flight, we examine changes in the spectrum through the ablation process.

27 - Which meteoroids are from asteroids and which are from comets?

Science Topic(s): Meteoroid Sources, Dynamical Evolution

Tam Do [student] (University of Western Ontario)
co-authors: Peter Brown

The parent body of meteoroids at Earth is central problem in meteor science. While generally, it is expected that denser particles are asteroidal and weaker particles are cometary, recent studies suggest that physical characteristics alone are insufficient for this dichotomous classification. We simulate orbital histories for ~400 mm-cm-sized meteoroids, including radiation pressure forces as well as gravitational, applying established orbital criteria to classify each as asteroidal or cometary at each integration timestep. High precision trajectory data, including orbital co-variance, are used to establish initial state vectors from two station observations using both the mirror-tracking system and electron-multiplying CCD cameras of the Canadian Automated Meteor Observatory. The resulting probability distribution of asteroidal or cometary origin is derived as a function of time. This allows for estimates of the change in orbital origin to be examined as a function of assumed meteoroid age. We focus on meteoroids with in-atmosphere velocities below 35 km/s, where asteroidal-cometary membership is often degenerate. Our goal is to estimate the fraction of asteroidal vs. cometary meteoroids purely based on dynamical evolution as a function of meteoroid age. Additionally, our analysis estimates mass inputs from meteoroids into Earth's atmosphere, categorized by origin.

28 - Chasing the Dragon: Forecasting the 2025 Draconids

Science Topic(s): Dynamical Evolution

Auriane Egal (Western University ; Planétarium de Montréal)
co-authors: Paul Wiegert, Peter Brown, Danielle Moser

The Draconid meteor shower has challenged modellers since its first recorded observation in 1926. Renowned for its unpredictable nature, it produces intense, short-lived outbursts that exhibit clear signs of mass segregation within the stream. As a result, some apparitions—like the 2012 storm—were only detected by radar instruments, while others were more prominent in optical observations. Due to its ability to reach storm-level activity, the Draconids may pose a significant risk to spacecraft safety. Yet accurate forecasting of the shower’s intensity remains difficult, owing to the erratic orbital history of its parent comet and limited constraints on the stream’s flux and particle size distribution. In this work, we present an updated model of the Draconid stream, building on the simulations of Egal et al. (2018, 2019). Our approach incorporates revised dust ejection scenarios and is calibrated using updated meteor measurements. In particular, optical and radar observations of the shower in 2019 and 2024 are used as additional constraints. We predict enhanced Draconid activity in 2025, caused by Earth’s encounter with the 2005 and 2012 trails ejected by comet 21P/Giacobini-Zinner. These results highlight the importance of continued multi-instrument monitoring of the Draconids to improve forecasting accuracy and underscore the value of coordinated observations during the 2025 apparition.

29 - Perth array results and future plan

Science Topic(s): Meteoroid Sources, In-situ Experiments and Spacecraft Anomalies

Hani Elbehiri [student] (Kochi University of Technology )
co-authors: Hany .S .Elbehiri, Islam Hamama, Eleanor K. Sansom, Iona Clemente, Hadrien Devillepoix, Yuichi Otsuka, Masa-Yuki Yamamoto

Infrasound waves are acoustic waves below human hearing that can propagate in the atmosphere for long distances. Infrasound waves could be generated from a variety of natural and human-made sources. Artificial sources of infrasound are chemical and nuclear explosions (Hamama et al., 2022), supersonic aircraft, rocket launches (Pilger et al., 2021), capsules such as the reentry of Hayabusa (Yamamoto et al., 2011), and wind turbines (Jakobsen, 2005). Natural sources, such as volcanic eruptions (Saito et al., 2021), microbaroms (Pichon et al., 2006), fireballs, and earthquakes (Hamama and Yamamoto, 2021). In September 2022, four INF04 infrasound sensors developed by Kochi University of Technology, Japan (KUT), were deployed near Perth, Australia. Fireballs were observed over the region and were captured by the Desert Fireball Network. Infrasound sensors from the current array had also recorded these fireballs. The FK analysis will be produced as a future plan for the current array data and future arrays after the redistribution of the infrasound sensor. Noise investigation of the different sensors’ sites will increase the signal-to-noise ratio with the current setup of the array, as we expect such observations could emphasize our understanding of the fireball detectability challenges. Additionally, the power spectral density will be produced for both the current and the future array to study the noise level for both sites.

30 - Hypervelocity Crateing and Disruption of Hydrous CM Chondrite and CI Simulant

Science Topic(s): Large impacts and Planetary Defence

George Flynn (State University of New York -- Plattsburgh)
co-authors: Melissa Strait, Daniel Durda, Robert Macke

The most mature asteroid deflection technique for monolithic asteroids ~100 m in size is kinetic impact. Two critical factors are the maximum velocity change (DVmax) in a single kinetic impact are momentum transfer by crater ejecta and the minimum impactor kinetic energy to fragment the asteroid, potentially leaving a fragment on a collision course. For any impactor speed (v), DVmax is limited by requiring the impactor kinetic energy be less than the minimum for onset of fragmentation (Q*), giving DVmax<2Q*B/v, where B is the ratio of impactor momentum to the momentum acquired by the target. There is little information on hypervelocity impact of hydrous targets. We performed hypervelocity cratering and disruption on the hydrous CM2 meteorite Aguas Zarcas and CI simulant prepared by laboratory hydrating ordinary chondrite material. For 4 to 5 km/s impacts Aguas Zarcas gave Q*=~600 J/kg, B=1.7, while the CI simulant gave Q*=210 J/kg, B=2.99. These give a DVmax=0.5 m/s for Aguas Zarcas and 0.25 m/s for CI simulant, much lower than the DVmax of 1.7 m/s we reported for the Northwest Africa 869 ordinary chondrite, indicating hydrous asteroids will be much more difficult to deflect without fragmentation than anhydrous asteroids.

31 - A Real-time All-Sky Fireball Camera Array Prototype for the Desert Fireball Network: Initial Results

Science Topic(s): Future Methods and Techniques

Dale Giancono [early-career researcher] (Curtin University)
co-authors: Hadrien Devillepoix, Robert Howie

All-sky cameras are widely used to capture data of fireballs during their bright flight. This enables trajectory calculation via triangulation of fireball streaks from multiple locations and determination of the meteoroid’s heliocentric orbit. Photometry calibrated to stars allows for ablation modelling. The Desert Fireball Network (DFN) employs all-sky fisheye cameras with GNSS-synchronised electro-optical shutters that interrupt exposures at 10Hz, producing arcminute-resolution imagery with sub-millisecond timing accuracy. However, challenges include smearing between segments, manual data reduction, and pixel saturation affecting bright fireball measurements. To improve on current DFN systems, a GNSS-synchronised all-sky video camera array has been prototyped. It detects and reduces data from optical transients in real-time using off-the-shelf cameras and standard computing hardware. It achieves sub-arcminute astrometric accuracy and can produce photometry of bright transients with a temporal resolution of 450Hz, with derived datasets such as light curves produced immediately. GNSS synchronisation provides sub-millisecond timing, and localised automatic gain/exposure control enhances the dynamic range of the system. Here, we present the initial findings and demonstrate the capabilities of this prototype through its first observed fireball events.

32 - A Case Study of Interstellar Material Delivery: Alpha Centauri

Science Topic(s): Influx of Interplanetary and Interstellar Material

Cole Gregg [student] (The University of Western Ontario)
co-authors: Paul Wiegert

The origins of detected interstellar material in our Solar System are unknown, as well as the details of its transport. Here we present a case study of the delivery of interstellar material to our Solar System from Alpha Centauri. This is a mature triple star system that likely harbours planets and is currently moving towards us, expected to have its closest approach approximately 28,000 years in the future. Assuming an ejection model for the system, we find that interstellar material with an Alpha Centauri origin can reach our Solar System and may currently be present here. The material that reaches us is mostly a product of low (<2 km/s) ejection velocities, and the rate at which it enters our Solar System is expected to peak around the time of Alpha Centauri 's closest approach. We estimate the current number of macroscopic Alpha Centauri particles (>100 meters in diameter) within our Oort Cloud to be 1E6, and during Alpha Centauri 's closest approach, this will increase by a factor of 10. The observable fraction, however, remains low. There is only 1E-6 probability that one of them is within 10 au of the Sun. A small number (~10) meteors (small particles >100 microns) from Alpha Centauri may currently be entering Earth's atmosphere every year: this number is very sensitive to the assumed ejected mass distribution, but the flux is also expected to increase as Alpha Centauri approaches.

33 - Constraining Meteor Entry Velocity from Radar or Incomplete Optical Observations

Science Topic(s): Meteoroid Sources, Meteoroid Impact Physics

Maria Gritsevich (University of Helsinki)
co-authors: Daniel Kastinen, Johan Kero, Eleanor Sansom, Alberto Castro-Tirado

Determining a meteoroid's pre-atmospheric velocity is critical for accurate orbit reconstruction and understanding source regions in the Solar System. However, radar systems such as high-power large-aperture (HPLA) radars often record only a portion of the meteor trajectory due to limited beam coverage and sensitivity constraints. Traditional methods that rely on full trajectory data or assume fixed initial velocities are often ineffective under these conditions. We present a physically based method for estimating pre-atmospheric velocity from partial meteor observations. By applying a dimensionless formulation of the meteoroid equations of motion, the initial velocity is treated as a free parameter and constrained using observed data. This approach avoids arbitrary assumptions and accounts for ablation, deceleration, and atmospheric density variations. The method is tested on radar observations from the MU radar in Japan and optical data from the Desert Fireball Network (DFN) in Australia. Results show that even with incomplete trajectory segments, the model provides reliable velocity estimates. Therefore such approach enables improved orbit determination using physically motivated models, particularly in cases where observational geometry or instrument limitations prevent full trajectory capture.

34 - Decadal Analysis of FRIPON Meteoroid Orbits and Their Association with Known Near-Earth Asteroids

Science Topic(s): Meteoroid Sources, Future Methods and Techniques

Meryem Guennoun [early-career researcher] (Oukaïmeden Observatory)
co-authors: François Collas, Jérémie Vaubaillon, Zouhair Benkhaldoun

Understanding the dynamical behavior of meteoroids and their linkage to parent bodies is fundamental to tracing their origin and predicting their activity. In this study, we analyze a 10-year dataset of meteor observations recorded by the FRIPON network to identify recurring meteoroid trajectories and investigate their potential association with known Near-Earth Asteroids (NEAs). Using orbital determination techniques and a dedicated parent body identification algorithm, we compared observed meteor orbits to the NEA catalog to search for dynamical similarities. Our analysis reveals several consistent orbital groupings that suggest the presence of meteoroid streams linked to specific asteroidal sources. These findings provide further evidence for the fragmentation and dust production activity of certain NEAs, while contributing to a better understanding of meteoroid stream formation mechanisms. The results not only refine our knowledge of meteoroid stream dynamics but also offer practical implications for meteor shower prediction and planetary defense. However, the accuracy of such associations remains a challenge. As previously discussed in Guennoun et al. (2023), traditional similarity criteria may lead to chance associations without rigorous statistical validation. Building on that work, we highlight the importance of incorporating uncertainty quantification and probabilistic testing in future parent-body identification efforts.

35 - Meteor Showers in Focus: Exposing Duplicates and Reclassification Needs

Science Topic(s): Meteoroid Sources, Dynamical Evolution

Maria Hajdukova (Astronomical Institute of the Slovak Academy of Sciences)
co-authors: Lubos1 Neslusan1, Regina2 Rudawska2, Silvia3 Durisova3, Tadeusz4 Jopek4

When Earth crosses a meteoroid stream once, it experiences a single meteor shower, intersecting it at both nodes produces two. Over time, planetary perturbations may form a filamentary structure of the Earth-crossing parts of the stream, which give rise to double, quadruple, or octuple showers from the same parent body. Conversely, a single shower can originate from two or more parent bodies. Non-gravitational effects also influence associated shower features. Therefore, along with the rapid increase in observations, characterizing a shower has become increasingly complex. With most showers lacking dynamical studies, classifying two with similar parameters is case-dependent. Whether they are considered independent or substructures of the same shower is largely conventional. However, no universal convention has been adopted. Authors submitting data to the Meteor Data Center (MDC) determine whether a newly observed shower is a discovery or matches a known one using their own criteria. As a result, the official IAU list of meteor showers includes duplicates and showers with multiple solutions that misrepresent the same shower. We analyzed 835 showers, identifying 7 duplicates, 43 multi-solution showers requiring reclassification, and 11 established showers needing status requalification. We also found 11 showers with mixed northern and southern solutions. The suggested corrections, once approved by the IAU F1 Working Group members, will appear in an updated MDC list.

36 - Infrasound Analysis of HTV Missions and Rocket Launches from Tanegashima Space Center, Japan

Science Topic(s): Human-generated Debris

Islam Hamama [early-career researcher] (National Research Institute of Astronomy and Geophysics)
co-authors: Masa-Yuki Yamamoto

Infrasound technology is increasingly utilized for detecting and tracking high-energy atmospheric events, including rocket launches. The H-II Transfer Vehicle (HTV) KOUNOTORI, which supplied the International Space Station from 2009 to 2020, offers a valuable case for studying infrasound propagation. This research focuses on acoustic signals from HTV launches at Tanegashima Space Center and their seasonal propagation conditions, particularly the potential for stratospheric ducting toward the Kochi University of Technology (KUT) Infrasound Sensor Network. Notably, HTV-06 to HTV-09 missions generated detectable infrasound at KUT, with some phases also captured by the IMS I30JP station. To address the complexity of rocket infrasound generation, a point-source approximation is applied to estimate source heights during various launch phases. Propagation modeling, including ray tracing and normal mode methods, is used to simulate expected celerities and transmission losses across altitudes. Results emphasize the importance of both near-field and far-field observations in capturing rocket-induced infrasound and highlight the role of modeling in interpreting signal arrivals at monitoring stations.

37 - Space Debris Re-Entries Over Australia: A Survey of Events, Environmental Risk, and Correlation with Earth Observation Imagery

Science Topic(s): Human-generated Debris

Benjamin Hartig [student] (Curtin University)
co-authors: Hadrien Devillepoix

With the increasing number of orbital objects, uncontrolled space debris re-entries are an emerging concern for environmental safety and human risk. This study cross-matches documented and suspected re-entry events over Australia with additional datasets to identify supporting evidence and potential validation methods. Particular emphasis is placed on correlating these events with available Earth Observation and All Sky imagery to aid in verification and impact location prediction. Additional verification against satellite and launch databases, such as Seradata, is explored. Australia's current capabilities, as well as limitations in civil debris detection and response, are also examined. The findings aim to lay a foundation for future development of technical frameworks for monitoring, evaluating and mitigating the risks related to space debris re-entries.

38 - Desert Fireball Network meets space junk: Capturing a Soyuz re-entry over Australia

Science Topic(s): Human-generated Debris, Future Methods and Techniques

Bella Hatty [student] (Curtin University)
co-authors: Eleanor K. Sansom, Hadrien A. R. Devillepoix, Martin C. Towner, Trent Jansen- Sturgeon

Jettisoned rocket stages and other scheduled debris can survive atmospheric re-entry and impact Earth. To mitigate risks, aviation authorities issue Notice to Air Missions (NOTAMs) that define expected impact times and areas. However, NOTAM verification is limited due to a global lack of observational coverage below altitudes of 200km. The Desert Fireball Network (DFN), a network of automated cameras across Australia, is designed and designated to track meteoroids and recover meteorites. While not purpose-built for monitoring re-entries, DFN cameras incidentally capture these events. On 7 August 2023, a Soyuz-2.1b rocket launched from Russia carrying a first-of-its-kind GLONASS-K2 satellite. The second stage, weighing 6.5t, was jettisoned ~30 minutes after launch. A NOTAM indicated the expected impact area spanned ~150,000km² between Tasmania and Macquarie Island. At 1356 UTC, a bright fireball was recorded by DFN cameras in Victoria and widely reported by eyewitnesses. We reconstructed the re-entry using DFN data to analyse the trajectory, fragmentation, and debris survivability. A dark flight model was applied to estimate impact times and locations, enabling direct comparison with the NOTAM. This provides rare suborbital-truth data to verify the re-entry. With increasing NOTAM frequency and orbital congestion, direct observations are critical. Our findings highlight the value of fireball networks and continued investment in ground-based monitoring.

39 - Dynamical history of κ Cygnid and August Draconid meteoroids

Science Topic(s): Dynamical Evolution

Filip Hlobik [student] (Comenius University in Bratislava)
co-authors: Jérémie Vaubaillon

August Draconids and κ Cygnids are two established meteor showers with large radiants close to each other in the August night sky. Some authors consider them a single Cygnid-Draconid complex, while others classify them as separate meteor showers. In this conference talk, we will present our ongoing work on the orbital evolution of κ Cygnid and August Draconid meteoroids from two nearby radiant groups. Our goal is to assess whether a dynamical connection exists between the two meteoroid streams, or if their radiant similarity is purely coincidental. To achieve this, we performed numerical integrations using the REBOUND integration package including non-gravitational radiation forces. For each simulated meteoroid orbit, we generated 10,000 clone particles in four different size bins (β ranging from 10⁻⁶ to 10⁻²) and integrated the system for 1,000 years into the past. Preliminary results do not show a high likelihood of a dynamical link between the two meteoroid streams. Both the κ Cygnid and August Draconid orbits are influenced mostly by close encounters with Jupiter, and 5:3J and 9:4J mean motion resonances, respectively.

40 - On the origin of our meteorites in the asteroid belt

Science Topic(s): Meteoroid Sources

Peter Jenniskens (SETI Institute)

This presentation is a summary of a recent review article published in Meteoritics & Planetary Science, co-authored with Hadrien Devillepoix. The article describes the first 75 meteorite falls for which an impact orbit could be calculated. Results show for the first time that different meteorite types arrive on different orbits. In particular, a cluster of H-chondrites arrived on orbits with a low inclination and semi-major axis beyond the 3:1 resonance, demonstrating that some H-chondrites originate from the Koronis asteroid family. The cosmic ray exposure age (CRE age) of these cluster around 6, 12 and 83 Ma, suggesting to us that all three young (< 100 Ma) Koronis clusters (Karin, Koronis_2 and Koronis_3) produced meteoroids that are now impacting Earth. Larger 1-km sized H-chondrite-like NEA originate from high in the asteroid belt, arriving via the 3:1 resonance, instead. Meteorites also arrive from that region, 4 of which have a 6 Ma CRE age. These may originate from the Nele asteroid family. There is also a source in the inner main belt with CRE ages of about 35 Ma. The Massalia family has a ~40 Ma cluster. L chondrites arrive mostly from a single source in the inner main belt, likely the Hertha family just above the Massalia family. LL chondrites originate from the Flora family, HED meteorites mostly from impacts on Vesta itself. Other possible source regions are also discussed.

41 - Late formation of the Oort Cloud based on CAMS meteor observations

Science Topic(s): Dynamical Evolution

Peter Jenniskens (SETI Institute)

This presentation is a summary of recent results from the CAMS low-light video meteor orbit survey. Over 2.7 million orbits were measured and the extracted meteor showers, their orbital elements and meteoroid physical data were published in the book "Atlas of Earth's Meteor Showers," one of two Association of American Publisher's 2025 PROSE Book Award Finalists in the category Chemistry, Physics, Astronomy and Cosmology. This data was analyzed for systematic differences between Jupiter-family and long-period comets and it was found that most long-period comets (from the Oort cloud) must have formed in the outer regions of the planetary disk, while most Jupiter-family comets sample a range of conditions throughout the disk. This implies that Neptune and Uranus scattered planetesimals into the Scattered Disk of the Kuiper Belt long before Oort-cloud orbits became stable enough to built an Oort Cloud. Both comet types are composed of cm-sized pebbles, which are released as meteoroids when the comets now return to the inner solar system. Those meteoroids decay over time into the smoke-like particles that form the zodiacal cloud, not by collisions but by thermal stresses based on the age of observed meteor showers in CAMS data.

42 - Investigation of the possibilities of simultaneous meteor observations from Russia and Tajikistan

Science Topic(s): Composition and Physical Properties, Meteor Physics and Chemistry

Anna Kartashova (Institute of Astronomy of the Russian Academy of Sciences)
co-authors: Kokhirova Gulchehra (1Institute of Astrophysics, National Academy of Ssciences of Tajikistan), Puzin Vasily (Institute of Astronomy of the Russian Academy of Sciences)

Meteor investigations have been conducted for a long time, but most of tasks solved by meteor astronomy are still actually. Meteor observations are needed to solve various tasks. Ideally, observations should be carried out around the clock and all year round (24 hours per day / 7 days per week / 365 days per year). It is more convenient to analyze the characteristics of both meteoroids themselves and their streams based on the same type of data. Therefore, the location of meteor (bolide) systems in different parts of the world is an approximation to the non-stop observation option. In order to implement a meteor network with stations spaced by longitude, to study their capabilities and work features, in 2024, the same type of meteor systems were launched on the territory of Russia and Tajikistan. Sony IMX 307 with 4 mm lenses are used for observations (with field of view of 87°x 45°), RMS software is used for observations and primary processing. Results of meteor observations and their analysis are presented. This work was supported by the Ministry of Science and Higher Education of the Russian Federation grant № 075-15-2024-626.

43 - Comet 289P/Blanpain and the Phoenicids: Disruptive Past Revealed

Science Topic(s): Meteoroid Sources

Toshihiro Kasuga (National Astronomical Observatory of Japan)
co-authors: N/A

Comet 289P/Blanpain, linked to the Phoenicid meteoroid stream, presents a compelling narrative. First spotted in 1819, it was lost for nearly two centuries. Its rediscovery stemmed from its orbital similarity to that of asteroid 2003 WY25, based on the observations and dust trail simulations of the 1956 Phoenicids. Despite its asteroid-like appearance in 2003, an observation in 2004 confirmed its cometary nature, revealing a faint coma and short tail. However, its current dust production rate is inadequate to account for the Phoenicid stream, suggesting a past disruptive event or extremely high activity perhaps around its 0.96au perihelion. In this talk, we present an observational study of 289P’s perihelion return in 2019-2020, utilizing near-infrared data from NASA's Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE) at two wavelengths: 3.4μm (W1) and 4.6μm (W2). The near-infrared images were obtained on two occasions: inbound (at 1.20au on UT 2019-10-30) and outbound (at 1.01au on UT 2020-01-11/12). The derived dust production rates, 0.01−0.02 kg s−1, are consistent with the earlier observation at 1.6au. This suggests a significant mass release event, likely due to the rapid rotational breakup of a precursor body between 1743 and 1819, produced fragments with a total mass equivalent to a 100m radius object. 289P is a remnant of a sub-kilometer precursor comet that may have been of low activity. This research is published as Kasuga (2025), AJ, 169, 54.

44 - The Origin of the Geminid Meteoroid Stream: Preliminary Results

Science Topic(s): Dynamical Evolution

Yung Kipreos [student] (University of Western Ontario)
co-authors: Yung Kipreos, Auriane Egal, Paul Wiegert, Peter Brown, Margaret Campbell-Brown, Pavel Spurný

The Geminid meteor shower is the strongest, and among the most extensively studied, annual meteor showers on Earth. Despite this, much about the Geminids remains a mystery, such as the origin and nature of its parent body, (3200) Phaethon. The difficulty in understanding the origin of the Geminid meteoroid stream is illustrated by the numerous modeling efforts that have struggled to replicate key observational features, including the shower duration, radiant, mass segregation, and bimodal shower activity. No current simulation has simultaneously reproduced all these observed characteristics of the shower. We aim to produce a model of the Geminid meteoroid stream that focuses on reproducing key observational features of the shower, using the stream modeling methodology established by Egal et al. (2018) with an emphasis on reproducing orbital elements of the stream derived from high-fidelity fireball observations (Borovička et al., 2022). In this presentation, we present the preliminary results of this work and discuss how these results give further context to the nature of the Geminid meteoroid stream.

45 - Analysis of pre-perihelion non-stationary activity of comet 12P/Pons–Brooks in 2023

Science Topic(s): Meteoroid Sources, Composition and Physical Properties

Gulchehra Kokhirova (Institute of Astrophysics, National Academy of Sciences of Tajikistan, *2Astronomical Institute of the Slovak Academy of Sciences)
co-authors: Marek Husárik*, Firuza Rakhmatullaeva, Oleksandra Ivanova*

Comet 12P/Pons–Brooks is a periodic comet with an orbital period of approximately 71 years. Because of the period duration, aphelion of 35.3 AU, and highly inclined orbit (74.2°), it classified as the Halley-type comet. The comet is considered the potential parent of the weak December κ Draconids meteor shower, which is active from late November to mid-December. In this work, we present the results of analysis of photometric and spectra observations of comet 12P, while this comet was at a heliocentric distance beyond 2.5 AU, before perihelion passage. Quasisynchronous observations were carried out from July to November 2023 using 0.61-m and 1.3-m telescopes Skalnaté Pleso Observatory (Astronomical Institute of the Slovak Academy of Sciences, IAU code 056), and 1-m telescope Zeiss-1000 Sanglokh International Astronomical Observatory (Institute of Astrophysics, National Academy of Sciences of Tajikistan, IAU code 193). Photometric observations were conducted using B, V, and R filters of the Johnsons-Cousins photometric system. During this period, the apparent (absolute) magnitudes and the Afρ(0°) values measured in the R filter indicate several outbursts in brightness and dust productivity. Comparision the dust production rate and the production rates of CN highlights that dust activity increased significantly as the comet approached the Sun, while gas activity exhibited more moderate changes.

46 - First results of meteor observations in Tajikistan within the Global Meteor Network project

Science Topic(s): Composition and Physical Properties, Influx of Interplanetary and Interstellar Material

Gulchehra Kokhirova (Institute of Astrophysics, National Academy of Sciences of Tajikistan)

Two sets of equipment for meteor observations in automatic mode were installed for the first time at the Institute of Astrophysics, National Academy of Sciences of Tajikistan. Test observations were conducted in Dushanbe and Sanglokh observatory and "first light" was obtained in June 2024. The video cameras are registered in the Global Meteor Network webpage and simultaneously operate in normal mode. We present information about the first results of meteor video observations in Tajikistan including a statistic of detection and meteors radiant-orbital data.

47 - Investigation of the δ-Cancrid Asteroid-Meteoroid Complex

Science Topic(s): Meteoroid Sources, Dynamical Evolution

Gulchehra Kokhirova (Institute of Astrophysics, National Academy of Sciences of Tajikistan)
co-authors: Ming1 Zhang1, X.-G.2 Li2, Abdulloi3 Zhonmuhammadi3, X.4 Liu4

The δ-Cancrid meteoroid stream forms four active meteor showers which are observable on the Earth annually during January-February and August-September. The stream’s definite parent comet has not been established. We performed a search for near Earth asteroids (NEAs) associated with this stream. We have followed the backward evolution of the orbital elements of a sample of NEAs and found their orbits at the Earth crossing positions. Using these orbits, we calculated the theoretical parameters of meteor showers associated with the considered NEAs. We carried out our search for observable active showers that match theoretically predicted ones with published data, and the result turned out that the predicted meteor showers of 13 NEAs were identified with the active showers produced by the δ-Cancrid meteoroid stream. The comet-like orbits of NEAs and established association with active meteor showers indicate their common cometary ori gin. The NEAs considered are moving within the stream and likely represent the dormant remnants of a parent comet of the δ-Cancrid asteroid-meteoroid complex disintegrated more than 12 thousand years ago.

48 - Classical Histogram Analysis of Radar and Optical Meteor Data: Key Points

Science Topic(s): Future Methods and Techniques

Svitlana Kolomiyets (1 - Astronomical Institute CAS in Ondřejov /2 - Kharkiv National University of Radio Electronics)

The histogram method remains a widely used tool in the analysis of meteor data, despite the emergence of more advanced statistical and computational techniques. In this study, we revisit this classical approach and evaluate its effectiveness when applied to datasets obtained via different observational methods. We present a comparative histogram-based analysis using two independent sources: radar data from the MARS system in Kharkiv (Ukraine) and photographic/video data from the Ondřejov Observatory (Czech Republic). The parameters analyzed include geocentric velocity (Vg), eccentricity (e), inclination (i), and several others — selected for their significance in meteoroid classifications and orbital dynamics. The shape of parameter distributions may vary depending on the observation method, as shown by previous studies and our results. Additional factors also contribute to these variations. A brief review of relevant research is included, and several open questions are briefly outlined. In summary, we outline key points regarding the strengths, limitations, and continued relevance of classical histogram analysis in the context of current and future interpretation of meteor data.

49 - Meteor clusters: tracing meteoroid fragmentation in near-Earth space

Science Topic(s): Composition and Physical Properties

Pavel Koten (Astronomical Institute of CAS, Ondrejov, Czech Republic)
co-authors: David Čapek, Juraj Tóth, Jeremie Vaubaillon, Aisha Ashimbekova, Simon Anghel

Meteor clusters are typically defined as groups of meteors that appear close together in both space and time. To date, only a handful of such events have been recorded instrumentally and analysed in detail. In all documented cases, thermal stress has been identified as the most likely cause of meteoroid fragmentation in the vicinity of Earth. In this talk, we summarize the known cases, present several new ones, and explore alternative scenarios of meteoroid fragmentation.

50 - Effects of meteoroid impacts as illuminators of lunar surface on water-ice stability

Science Topic(s): Impacts on Other Planets/Surfaces

Jack Lopes [student] (University of Western Ontario)
co-authors: Paul Wiegert

With the upcoming Artemis missions to the lunar south pole, there is much to learn about the environment ahead. This research examines the stability of water-ice on the lunar surface under solar illumination and meteoroid impacts. Key questions include how much ice can exist, where it is located, and the rate at which it is removed. To investigate these factors, I developed a ray-tracing simulation that models surface illumination and energy deposition. A key test of the simulation is the precise identification of Permanently Shadowed Regions (PSRs), identified by other authors which provide an ideal test scenario for isolating meteoroid impact effects. The simulation can also model "illumination" by sporadic meteor sources or other meteoroid populations. By quantifying the energy deposition as a function of impact parameters, this work refines our understanding of energy flux across the lunar surface. After extracting the flux expected from meteoroid sources, two quantities are of primary interest. First, I estimate the timescale for a region to be fully cratered based on known meteoroid flux values. Second, I investigate impact-driven energy deposition, considering total flux and per impact energy. By comparing this to the sublimation energy of water-ice, I aim to determine the rate of ice loss due to meteoroid impacts within PSRs. These calculations focus on sub-millimeter sporadic meteoroids, considered the dominant contributors to overall flux at these sizes.

51 - Mitigating meteoroid impact risk and preparing future instrumentation

Science Topic(s): In-situ Experiments and Spacecraft Anomalies, Meteoroid Impact Physics

Mark Millinger (European Space Agency)

The European Space Agency (ESA) recognises meteoroids as a relevant risk for space assets. Therefore a wide range of activities is performed to model, predict and mitigate these risks. The activities cover inter alia environment model development, impact effects testing and simulation, risk assessment tool development, risk mitigation methods and instrument development. This talk will give an indicative overview of all meteoroid impact risk related activities with the main focus on instrument feasibility and development activities. Note that typically particle sizes of hundreds of microns are necessary to pose a risk to spacecraft. Therefore many recent developments target the 0.1-10 mm size range. However, more scientific instrumentation is also in preparation, as in particular ASTERIA (Active Sensors for Telemetry of Extraterrestrial Impacts at Gateway).

52 - Ongoing Investigations with the Lowell Observatory Meteor Camera Network

Science Topic(s): Meteoroid Sources, Composition and Physical Properties

Nicholas Moskovitz (Lowell Observatory)
co-authors: Samantha Hemmelgarn, Peter Jenniskens, Denis Vida

Our group at Lowell Observatory maintains a network of nearly 100 meteor cameras (optical video) distributed across 8 sites in northern Arizona. This network has been developed around both CAMS and GMN components. Data are processed locally as well as reported externally to both of those larger projects. Given the dark skies across much of Arizona and nearly 300 clear nights per year, our network has been highly productive yielding ~100,000 meteor orbits annually. We will present the status of the Lowell network including plans for expanding the number of cameras, and recent studies that leverage the resulting data products. The first of these studies investigated the relationship between long period comets and their associated meteor showers (Hemmelgarn et al. 2024, PSJ 5, 242). We found that the orbital properties of a meteor shower can be used to predict the location on sky (RA, Dec) of the parent comet with sufficient accuracy so as to guide the discovery of new meteor shower parent bodies with wide field telescopic surveys, e.g. the upcoming Vera Rubin Observatory Legacy Survey of Space and Time (LSST). The second study is an ongoing investigation that leverages machine learning to classify meteors based solely on observed properties. This approach uses principal component analysis and clustering algorithms to define a classification scheme analogous to traditional methods that map observed properties to material properties, e.g. the kB parameter.

53 - Proposal of a new long life mechanism of meteor persistent trails

Science Topic(s): Composition and Physical Properties, Meteor Physics and Chemistry

Nagatoshi Nogami (International Meteor Organization)
co-authors: Shinsuke Abe

Some light emission mechanisms of meteor persistent trails have been proposed until now. But because they are based on physical por chemical processes with atoms and/or molecules and their ions, their quite short life time didn't satisfy to explain the emission keeping more than several ten seconds. To this solution we propose a process of "thermoluminescence" of soldified ablation droplets based on the solid state physics. In the meteoroid droplet consisted of silicates minerals, electrons in the valence band are excited by the ablation heat and emit light when they drop to the ground state. The excited electron forming an "exciton" with a hole are trapped at around structural defects in the silicates. This behavior is characteristic of our mechanism. A couple of important factors to the lifetime are also discussedin the presentation.

54 - Planetary Defence Activities at ESA’s Planetary Defence Office

Science Topic(s): Large impacts and Planetary Defence

Francisco Ocaña (Planetary Defence Office / ESA / Deimos)
co-authors: Marco Micheli, Luca Conversi, Richard Moissl

ESA’s Planetary Defence Office is a specialised division within ESA dedicated to protecting Earth from asteroid threats. This presentation focuses on the Office activities, especially those related to the smaller end of the NEO size distribution, and on the understanding of NEOs as parent bodies of meteoroids. The Office is structured in three main pillars: Observations: Follow-up observations are conducted using our telescope network. Moreover, the Agency is already testing the first Flyeye telescope to perform a wide-field discovery survey, increasing our capabilities to find nearby objects and potential imminent impactors. In space, ESA is working on NEOMIR, an infrared telescope to detect imminent impactors coming from the direction of the Sun (e.g., Chelyabinsk). Information provision: Long-term impact likelihood estimations in a Risk list (by Aegis), and monitoring the imminent impactors (by Meerkat -- like the recent 2024 BX1, 2024 RW1…). Mitigation: activities in order to understand the risk in case an impact may happen. The main activity is the HERA mission, tasked to observe the results of DART impact. Meanwhile we are preparing RAMSES to study how Apophis behaves in the nearby approach to the Earth. Among other projects, we have 3 AMS all-sky cameras monitoring nighttime sky, we are working on an algorithm to exploit Meteosat MTG-LI fireball data and we are restarting the lunar impact flashes monitoring.

55 - Comparative analysis of meteor spectra observed simultaneously from multiple locations

Science Topic(s): Composition and Physical Properties

Veronika Pazderová [student] (Comenius University in Bratislava)
co-authors: Pavol Matlovič

Meteor spectroscopy serves as the primary method for investigating the composition of meteoroids, providing insights into both their general elemental makeup and the relative abundances of individual elements. Over the past decade, the Slovak AMOS (All-sky Meteor Orbit System) network, managed by researchers from Comenius University in Bratislava, has amassed an extensive dataset of meteor spectral observations. Among these, a significant number consist of multi-station spectra documenting the same meteor events. Despite capturing the same object, these observations often exhibit notable variations. This study focuses on the comparative analysis of multi-station spectra for selected meteors, exploring potential factors contributing to their discrepancies.

56 - Understanding the Antarctic/Greenland dust deposits with meteoroid models

Science Topic(s): Meteoroid Sources, Dust Particles and Clouds in the Solar System and Beyond

Petr Pokorny (The Catholic University of America/NASA GSFC)
co-authors: Diego Janches, Juan Diego Carrillo-Sánchez

We investigate two disagreements between meteoroid models in the inner solar system and observed quantities at Earth: D1: The lack of particles smaller than 100 micrometers in Antarctic meteoroid collections that are predicted by meteoroid models and the disagreement between the meteoroid model mass flux at Earth, and D2: the amount of meteoritic smoke deposited in the polar regions of Earth (Brooke+ 2017). To address these disagreements, we used the dynamical models for Jupiter-family comet (JFC) main belt asteroid (MBA) dust populations (Pokorny+ 2024). To address D1, we analyzed the model parameters for both dust populations separately: the initial size-frequency distributions and the collisional strength of particles. This provided us with a suite of model representations that we compared to SFDs and accretion rates in Rojas+ 2021. We find that the population mixing ratios from Carrilo-Sanchez+ (2020) match well the reported SFD in Antarctic deposits (Genge+ 2020). To address D2, we additionally implemented the long-period models available from (Pokorny+ 2014, 2019). Currently, the work is ongoing, and we will present our preliminary results that show the current model-to-data disagreements and potential solutions.

57 - Lateral spreading of meteoroids fragments

Science Topic(s): Meteoroid Impact Physics

Olga Popova (IDG RAS, Moscow)
co-authors: Elena Podobnaya

The sizes of scattering and/or crater fields on planets with atmospheres are determined by atmospheric sorting and the interaction of fragments with each other after disintegration. Small fragments may be affected by wind. This interaction results in an additional lateral velocity, which is directed perpendicular to the entry velocity. Theoretical estimates of this velocity differ significantly and require further clarification. There are over 1400 freshly formed impact sites on Mars created by meter-scale meteoroids. There are 20 nearly twin craters, and 70 pairs, the craters in which differ in diameter (up to 13 times). Twin craters represent the simplest case of the disintegration of a meteoroid, where the intercrater distance is determined by the fragment interaction. Twin craters provide ideal observational data for comparison with theoretical estimates of fragment spreading. Pairs of different craters provide further verification of these estimates. Study of the intercrater distance provides a possibility to roughly estimate the impactors density and their possible fraction in the whole meteoroid population. The presentation will demonstrate the results of numerical modeling of the impactors of different origin entering the Mars atmosphere at different angles and their further disintegration into two fragments, will show how meteoroid parameters affect the dispersion of fragments, and will compare them with observational data.

58 - Ten years of the digital Desert Fireball Network - from meteorites to space debris

Science Topic(s): Future Methods and Techniques

Eleanor Sansom (Curtin University)
co-authors: Hadrien Devillepoix, Benjamin Hartig, Martin Cupak, Sophie Deam, Dale Giancono, Iona Clemente, Thomas Stevenson

For the past decade, the digital Desert Fireball Network (DFN) has been observing Australian skies for material entering Earth's atmosphere. We will present an overview of the DFN's evolution and plans for the future, as well as the achievements and scientific output of the Fireballs team at Curtin University. Building on a small array of analogue systems (based on those of the original European Fireball Network), the autonomous observatories and software pipelines of the digital DFN allowed for rapid expansion. It is the foundation of the Global Fireball Observatory, which has grown into a global collaborative initiative. The DFN has captured over 2000 fireball events, leading to the successful recovery of eight meteorites with known orbits in Australia, facilitating 17 recoveries across the GFO. The fireballs team have iteratively built software for trajectory analysis, orbit determination, and atmospheric interaction modelling. Our latest work using drone surveys and machine learning is facilitating remote meteorite recoveries. The DFN is also capable of observing re-entering space debris, and providing expertise into Space Domain Awareness areas. We are now looking toward the next decade, with ever growing collaborative opportunities. With the increase of imminent impactor detections, we are aiming to bridge the gap between asteroid science and meteorite geochemistry.

59 - Observation of the Outburst of the Tau-Herculid Meteor Shower in 2022

Science Topic(s): Dynamical Evolution

Mikiya Sato (National Astronomical Observatory of Japan)
co-authors: Jun-ichi Watanabe, Chie Tsuchiya, Ryuichi Hasuo, Hitoshi Hasegawa, Ichi Tanaka, Toyokazu Uda, NHK Cosmic Front Crew

The tau-Herculid meteor shower (TAH, #61) originates from Comet 73P/Schwassmann-Wachmann. The meteor outburst of the tau-Herculids in 2022 was predicted by several researchers, including the presenting authors, to be caused by dust trails formed from 73P. Among these, the dust trail released in 1995 was of particular interest, as the parent comet, 73P/Schwassmann-Wachmann, underwent a huge outburst and fragmentation that year, likely dispersing a substantial amount of dust particles. Therefore, we devised an observation plan to detect the peak activity of the tau-Herculids, which was expected to originate from the 1995 dust trail. Since the predicted peak was at about 5:00 UT on May 31, 2022, we decided on the observation in California, where conditions were favorable for observation of the predicted peak. Wide-field video observations detected a peak at 4:46 UT, with a simple hourly rate reaching over 170. The flux at that time was measured to be 6.1±0.93×10^-3 per km^2 per hour. Furthermore, a live streaming fixed-point camera (Subaru-Asahi Star Camera) at the Subaru Telescope site on Maunakea, Hawaii, began detecting meteors from this shower approximately 90 minutes after the peak. The camera continued to monitor the shower as its activity gradually declined. In addition, it captured a small number of meteors associated with the shower on the nights before and after the peak night. This presentation provides a detailed report on these observations.

60 - Debiasing Meteoroid Flux Estimates Using the Desert Fireball Network's Clear-Sky Survey

Science Topic(s): Influx of Interplanetary and Interstellar Material, Future Methods and Techniques

Konstantinos Servis [student] (Curtin University)
co-authors: Hadrien Devillepoix, Ellie Sansom, Thomas Stevenson

The Desert Fireball Network (DFN) is a global network of autonomous observatories designed to capture fireball events and reconstruct their trajectories and orbits. To accurately estimate meteoroid flux density, we developed a methodology for debiasing observations using a clear-sky survey based on HEALPix sky partitioning. This approach quantifies observable areas and time under clear conditions. We analyzed DFN observations from 2015, calculating the clear-sky time-area product and validating the method using the Southern Taurid meteor shower. The cumulative size-frequency distribution of meteoroids was fitted with a two-segment power-law model. A discontinuity was observed but identified as an artifact of dataset incompleteness. For higher masses, results align with previous studies, confirming the method's robustness. This automated approach provides precise meteoroid influx estimates and is effective for analyzing large datasets, including focused streams like the Southern Taurids. By integrating clear-sky conditions and leveraging HEALPix, this work advances our ability to study meteoroid populations and their anisotropies.

61 - Searching for tidal disruption signatures amongst NEAs and impact data

Science Topic(s): Meteoroid Sources, Dynamical Evolution

Patrick Shober [early-career researcher] (NASA)

In this study, we search for tidal disruption signatures amongst 22,424 sporadic asteroidal impacts spanning millimeter to multimeter sizes. Our cluster search focuses on recent disruptions, occurring within the 10–50 kyr orbital decoherence window, the average amount 'decoherence lifetime' of near-Earth streams (Pauls & Gladman 2005; Shober et al. 2025 A&A)—is manifest. Our cluster analysis finds a minor excess of similarity for DH<0.01 for the CAMS, GMN, and EDMOND databases, which matches nicely the observed excess found for NEAs in Shober et al. 2025 in A&A. However, when searching for a "long-term" tidal imprint in the perihelion distribution, we do not observe the expected concentration near 1 au predicted by tidal disruption models (Granvik & Walsh 2024). While we do find a strong excess at q≈1 au, but it diverges from pattern expected resulting from tidal-disruption. Instead, this concentration of perihelion values near 1 au in the meteor datasets are more likely explained by the preferential survival of objects that have avoided repeated low-perihelion encounters—and thus remain less thermally processed (Shober et al. 2025 Nature Astr.). Recent work indicates that meteoroids undergoing multiple close passes to the Sun fragment rapidly, effectively biasing the impact dataset toward 1 au survivors. Our results, therefore, suggest that meteoroid thermal degradation, rather than ongoing tidal disruption, drives the observed perihelion distribution amongst meteors.

62 - The 20 May 2023 bolide over Australia: Ground-to-space observations

Science Topic(s): Large impacts and Planetary Defence, Meteoroid Impact Physics

Elizabeth Silber (Sandia National Laboratories)
co-authors: Eleanor Sansom2, Miro Ronac Giannone1, Loring Schaible1, Hadrien Devillepoix2, Thomas Edwards1, Mark Boslough3, Iona Clemente2, Denis Vida4, and Damir Šegon5, Vedant Sawal1

Very bright meteors, also referred to as fireballs and bolides, are generally produced by objects >10 cm in diameter. While impacts by large asteroids (10s of meters in diameter) are relatively rare, they are not statistically negligible. Thus, the characterization of these objects is of utmost importance, and helps shed light on why some events might result in more catastrophic outcomes than others. We present the ground-to-space observations of an energetic fireball that resulted in an airburst over Australia on 20 May 2023. The fireball entered with a speed of 28 km/s over Queensland at 09:22 pm local time, and underwent a catastrophic disintegration at an altitude of 29 km. It deposited energy of ~7.2 kt of TNT equivalent (1 kt = 4.184·1012 J), making it one of the top 20 most energetic bolides detected by the US government sensors and reported in the JPL/NASA CNEOS database since 1988. The bolide was so bright that it was visible at a distance of 600 km. It saturated ground-based cameras, stifling efforts to derive the full trajectory and obtain photometric measurements. We found infrasound signals at four infrasound stations as far as 6000 km away. We will present observations of this energetic fireball event and discuss implications for planetary defense and characterization of similar events. SNL is managed and operated by NTESS under DOE NNSA contract DE-NA0003525.

63 - Finding Fireballs in Lightning: A Daily Pipeline to Find Bolides in GOES Weather Satellite Data

Science Topic(s): Influx of Interplanetary and Interstellar Material, Large impacts and Planetary Defence

Jeffrey Smith (SETI Institute)
co-authors: Robert L. Morris, Randolph Longenbaugh, Jeffrey Olson, Jessie Dotson

Weather satellite data contains a wealth of information far beyond its application to the weather. The GOES lightning mapper instruments observe millions of lightning strikes per day and a handful of bolides (bright meteors). Our team has succeeded in creating an efficient pipeline to identify the bolides. Our algorithms are also sensitive to other interesting phenomena. Funded by NASA's Planetary Defense Coordination Office (PDCO), our goal is to create a calibrated and statistically consistent data set of bolide light curves to inform the planetary defense community of the risks associated with large asteroidal impacts, but the data set can also be useful for other meteoroidal studies. We utilize a three-stage detection pipeline, with successively more computationally expensive algorithms: 1) simple Hierarchical Clustering, 2) Random Forests and then 3) Convolutional Neural Networks. Detections that cannot be published automatically are deferred to a human subject matter expert who uses an intuitive web-based GUI to perform final assessment. Detections are promptly published on a NASA hosted publicly available website, https://neo-bolide.ndc.nasa.gov. We present the evolution of our pipeline, the ML techniques utilized and how we continue to incorporate new information to improve detection performance. We will discuss how to access our data, the distribution of events we have detected and how our data set can be utilized in conjunction with other meteor data sets.

64 - Comparing Mechanical Strengths of Real and Simulated Meteoroids

Science Topic(s): Composition and Physical Properties, Meteor Physics and Chemistry

Thomas Stevenson [student] (Curtin University)
co-authors: Ellie Sansom, Hadrien Devillepoix

Key mechanical properties of extraterrestrial objects are typically constrained using meteorites that have impacted Earth, especially those whose trajectories have been reconstructed by fireball cameras. Meteorites are problematic because they represent only the strongest fraction of objects entering Earth’s atmosphere. Most objects are completely vaporised and rendered unavailable for direct testing. For complete understanding, it is necessary to survey as much incoming material as possible, not only the strongest surviving fragments. For every meteoroid with a reconstructed trajectory, a pressure-factor or Pf value can be derived that indicates its resistance to destruction. A high Pf value denotes a tough, siliceous or metallic object that is likely to drop a meteorite. Successively lower Pf values indicate carbonaceous objects, cometary remnants, and unconsolidated rubble piles. We have calculated Pf values for approximately 60 meteorite falls and a range of objects of unknown composition detected by the Desert Fireball Network from 2014-2024. Against this dataset, we compare simulated populations of meteoroids generated by a combined analytical ablation simulator and stochastic fragmentation simulator. The purpose of this presentation is to demonstrate the utility of Pf values in characterising meteoroids, and to discuss how fireball observations can reveal details of meteoroid composition and structure.

65 - AMOS global meteor network - status and results

Science Topic(s): Composition and Physical Properties

Juraj Toth (Comenius University in Bratislava, Faculty of Mathematics, Physics and Informatics)
co-authors: Juraj Toth, Pavol Matlovic, Leonard Kornos, Tomas Paulech, Pavol Zigo, Martin Balaz, Tomas Voros, Maria Paprskarova, Filip Hlobik, Adriana Pisarcikova, Veronika Pazderova and Jaroslav Simon

AMOS (All-Sky Meteor Orbit System) is an automated, intensified meteor detection system operating in both the Northern and Southern Hemispheres, monitoring meteor activity 24/7 in the optical range up to +4 magnitude, mainly in mid range of meteor brightness from -3 to +2 magnitude. We present the current status of network of 17 all-sky and 17 spectral stations. The system was invented and developed by Comenius University in Bratislava to detect and characterize weak meteor showers and to provide comprehensive information about the dynamical and physical nature of meteoroids in the millimeter to decimeter size range worldwide. AMOS operates in collaboration with several institutions, including the IAC (Canary Islands), SpaceObs and Paniri Caur Observatory (Chile), the University of Hawaii and SMA, Curtin University in Perth, and the Cederberg and Rogge Cloof Observatories in South Africa, and recently a new spectrograph installed in partnership with the Vatican Observatory in Arizona. We present results of notable meteor showers, special meteor events as meteor clusters, and case studies aimed at the detailed dynamical and physical characterization of selected meteors with achondritic signs, including analysis of their spectral properties.

66 - Use of event-based camera for meteor science

Science Topic(s): Future Methods and Techniques

Jeremie Vaubaillon (LTE, Paris Observatory)
co-authors: Laure Acin, Aisha Ashimbekova, Meryem Guennoun, Camille Simon-Chane, Aymeric Histace

Today optical meteor cameras are limited by the image rate usually set to standard video values. The increase the signal pace usualy comes with a loss of sensitivity. Event-based cameras potentially offers high signal rate (up to 10 kHz in theory) and similar spatial resolution as regular cameras. Here we present the first tests of such cameras for meteor sciences. We highlight the strengths and weaknesses of such device, and provide recommendation for future usage for meteor science.

67 - Modelling of faint meteors and bolides using AMOS all-sky data

Science Topic(s): Composition and Physical Properties, Meteor Physics and Chemistry

Tomáš Vörös [student] (Comenius University)
co-authors: Mária Paprskárová, Pavol Matlovič, Juraj Tóth

The AMOS network of all-sky cameras is currently operating in six countries, spanning both hemispheres. In the past years we have collected vast amounts of data that contain precious information about meteoroids with masses ranging from less than a gram to tens of kilograms. Currently, we are developing tools for analysis of the recorded footage. Our presentation will be divided into two parts. Firstly, we will talk about fainter meteors that we simulate using the model of meteoroid erosion by Borovička et al. (2007). We will show some preliminary results of our work, with our ultimate goal being characterisation of the most prominent meteoroid streams and their parent bodies. Secondly, we will present our analysis of several selected bolides. We model them focusing on the gross-fragmentation process, in order to examine its connection to the meteoroid's type and changes in the ablation rate. Following the fragmentation, we study the size and spatial distribution of released fragments, taking into account the atmospheric conditions strongly affecting the behaviour of smaller grains. For cases large enough to potentially produce meteorites, we will present strewn fields predicted by our approach.

68 - Physical characteristics of shower meteoroid inferred thought Dynamic Nested Sampling

Science Topic(s): Composition and Physical Properties, Future Methods and Techniques

Maximilian Vovk [student] (Western University)
co-authors: Peter Brown, Denis Vida

Meteoroid impacts threaten satellites, demanding accurate estimates of meteoroid physical properties. We introduce Dynamic Nested Sampling as a robust probabilistic method for inverting and quantifying uncertainties in meteoroid characteristics from optical data. Our approach uses the erosion fragmentation model by Borovička et al. (2007), where meteoroids lose mass by ejecting micrometer-sized grains that ablate independently. We observed Orionids, Alpha Capricornids, and Draconids using EMCCD cameras and the Canadian Automated Meteor Observatory (CAMO) mirror tracking system. EMCCD cameras achieve an approximate limiting magnitude of +7, ~50 m per pixel resolution at 100 km, and 32 FPS. The CAMO system offers similar sensitivity but 6 m per pixel resolution at 100 km and 100 FPS, providing high cadence details of meteoroid fragmentation and morphology. The Dynamic Nested Sampling method is used to fit the erosion model to the data and invert realistic uncertainties. The method is given wide priors to minimize assumptions on the physical properties (especially bulk density), thoroughly exploring parameter space and avoiding local minima. Our preliminary results show robust propagation of measurement uncertainties and reveal how model outcomes depend on measurement precision. We also observe a fundamental limit to model-inversion accuracy, determined by the meteoroid’s morphology as captured by CAMO.

69 - The Pan-STARRS search for Near-Earth Objects

Science Topic(s): Large impacts and Planetary Defence

Richard Wainscoat (University of Hawaii, Institute for Astronomy)
co-authors: Robert Weryk

The Pan-STARRS telescopes, located on Haleakala, in Maui, Hawaii, have been conducting a survey for Near-Earth Objects since 2014. They have become one the leading surveys for Near-Earth Objects. Each night the telescopes acquire sequences of four observations of areas of the sky, spaced over a period of approximately 1 hour. Each night, each of the two telescopes images approximately 1,000 square degrees of sky, typically to a limiting magnitude of V~22 when there is no bright moon in the sky. The observations are optimized for discovery of larger Near-Earth Objects, but serendipitous observations of meteoroids inevitably happen. These may be seen as streaks in images as an object burns up in the atmosphere, or as a sequence of shorter streaks showing significant acceleration in motion if a larger sized meteoroid is seen shortly before impact. For the most part, longer streaks are ignored in Pan-STARRS data, because they typically correspond to artificial objects. Over the next few years, efforts will be made to make the Pan-STARRS observations publicly available. The areas of the sky surveyed are already published to the Minor Planet Center, In the shorter term, we are open to requests to search for specific meteoroids in the survey data. With a typical image quality of 1”, we have a spatial resolution of ~2 m at 400 km range, the minimum for good focus. However, this does suggest that a bright and laterally fragmented meteoroid may be resolvable as separate trails.

70 - Meteor showers as a tool to investigate evolutionary history of the parent comets

Science Topic(s): Meteoroid Sources

Junichi WATANABE (National Astronomical Observatory of Japan)
co-authors: Mikiya Sato

The density of the meteoroids in a dust trail depends generally on the activity of the parent comet when the dust trail was formed. There should be a correlation between the scale of a meteor shower appearance and the activity of the comet. In fact, we found the correlation between the activity of the October Draconids and Comet 21P/Giacobini-Zinner (Watanabe & Sato 2008). Therefore, by studying the scale of a meteor shower on a specific date and time, we can estimate the activity of the comet at the time when the corresponding dust trail was formed. Namely meteor showers can be used as a tool to investigate the past activity of the parent comet. In this study, we applied this method to the Phoenicids and studied the history of the activity of the parent comet 289P/Blanpain. While this comet was thought to be very active during the 18th and 19th centuries, which caused the strong display of Phoenicids in 1956, it was estimated to become less inactive by 90% (Fujiwara et al. 2017) or by 80% (Sato et al. 2017) between 1909 and 1930 than the previous century. Although it displayed a huge episodic outburst in 2013 despite its heliocentric distance of 3.9 au (Ye & Clark, 2019), it seems to become dormant again after this event (ex. Kasuga 2025, Ye et al. 2021). By increasing the number of such observational samples, it should be possible to understand the physical evolutionary history of the parent comet by investigating the activities of the corresponding meteor shower.

71 - Pan-STARRS and the search for Potentially Hazardous Comets

Science Topic(s): Influx of Interplanetary and Interstellar Material, Large impacts and Planetary Defence

Robert Weryk (The University of Western Ontario)
co-authors: Richard Wainscoat

Pan-STARRS is a leader in Near-Earth Asteroid (NEA) discovery. We also find a large fraction of new comets which will one day become the dominant impact hazard to Earth after more of the NEA population is known. The motion of an object, observed as a tracklet -- a short sequence of observations -- is used to estimate how interesting it is, by comparing it to the motion of a typical main belt asteroid. This is done by computing a score (0-100) which must exceed 65 to receive targeted follow-up. While comets are found mainly based on their morphological appearance -- they are "fuzzy" -- a larger score subjects them to more scrutiny. However, comets farther away have slower motion, which causes them to self-subtract in difference images used by processing pipelines. Some comets (and Manx objects) may not have visible tails, which also hinders their discovery. To increase our comet discovery rate, we now process "chip" images. In addition to a fainter sensitivity limit, having more slow-moving comet tracklets allows linking them based solely on their motion, allowing for improved visual review of objects selected only by their orbital parameters instead of their scores. Pixel analysis for these candidates can also reveal low-level activity below what is obvious from a visual review alone. For new comets, this may lead to meteoroid streams at Earth being expected long before their formation, allowing for meteor observing campaigns to study their physical and chemical properties.

72 - Infrasound observations for 3 SRC reentries as well as multiple configuration experiments with MOMO sounding rockets and STRATOVISION baloons

Science Topic(s): Meteor Physics and Chemistry, In-situ Experiments and Spacecraft Anomalies

Masa-yuki Yamamoto (Kochi University of Technology)
co-authors: Yasuhiro Nishikawa, Yuta Hasumi, Yusuke Yasukochi, Yuichiro Inoue, Kazuki Mizuno, Eleanor Sansom, Hadrien Devillepoix, Elizabeth Silber, Islam Hamama, Hani Elbihiri, Mario Batubara, Norihisa Segawa, Hiroaki Saito, Yoshihiro Kakinami, Yoshiaki Ishihara, Yoshihiro Hiramatsu, Masafumi Edamoto, Hiroki Kono

Infrasound observation is commonly used for energy estimation of meteorites entries. For the limited occasions of hypersonic reentries from the interplanetary space: Hayabusa (2010), Hayabusa2 (2020), and OSIRIS-REx (2023) reentry events were used for multiple site ground observation campaigns for infrasound detection of hypersonic shock waves coming from their trajectories. During these two decades, trials for comparing between seismic and infrasound sensors for confirming air-to-ground coupling process for Hayabusa reentry, expanding 7 multiple arrays with 28 INF04 infrasound sensors beneath Hayabusa2 reentry trajectory, and comparable observation with Hayabusa2 case as a part of huge observation campaign for OSIRIS-REx were carried out, then datasets were compared with specific designs of capsules and physical parameters of reentries. The other experiments were tried in Japan with using private company’s sounding rocket of MOMO series developed by Inter Steller Technologies (IST) as well as controlling fly-back small balloon systems by STRATOVISION for in-situ observation of infrasonic and audible sound in stratosphere, mesosphere, and lower thermosphere. Shock waves were successfully detected for MOMO experiments with small onboard infrasound sensor of INF03S and multiple INF04 sensors on ground. In this talk, we will introduce briefly about Kochi University of Technology’s most recent activities.

73 - Droppers in good and bad places: three years of fireball monitoring in Oman

Science Topic(s): Influx of Interplanetary and Interstellar Material, Meteorite Recoveries

Anna Zappatini [student] (University of Berne, Switzerland)
co-authors: Anna Zappatini, Urs Eggenberger, Beda Hofmann, Edwin Gnos, Beat Booz, Mohammad Tauseef, Martin Bucher, Manuel Eggimann, Frank Gfeller, Pascal Kruttasch, Sebastian Lindemann, Mohammed Al-Qassabi, Hussain Al-Ghafri, Abdulmunaim Al-Zakwani, Muati Al-Muati, Hadrien Devillepoix, Eleanor Sansom, Martin Cupák

Since 2022, fireball cameras from the Desert Fireball Network (DFN) have been observing the night skies over Oman. The six cameras monitor an area of approximately 200,000 square kilometres of mostly bright and barren desert plains — excellent search terrain that is ideal for finding even small meteorites. Over the past three years, the Omani Meteorite Monitoring Project (OMMP), which is part of the Global Fireball Observatory (GFO), has recorded numerous meteors. Two fireball observations have resulted in the successful recovery of the corresponding meteorites. We will place these meteorite falls in the context of the monitoring time and the total number of meteors observed over Oman. We will also discuss cases where meteorites could not be recovered, highlighting the challenges faced and the lessons learned throughout the project.

74 - A novel approach for revealing dynamical disintegration of irregular-shaped meteoroids with particle-sintered model

Science Topic(s): Dynamical Evolution

Ziwen Li [student] (Beijing Institute of Technology)
co-authors: Xiangyuan Zeng

Meter-sized meteoroids, typically originating from loose rubble-pile asteroids, feature irregular geometries, heterogeneous structures, and relatively high strength. Previous models oversimplify them as homogeneous spheres, failing to explain phenomena such as fragmentation behaviors that deviate from Weibull-like scaling laws. This study proposes a novel method based on the Discrete Element Method (DEM) to capture the structural and dynamical evolution of meteoroids during atmospheric entry. This model integrates aerodynamics, 6-DOF motion, structural strength, and ablation, using adjustable sintered bonds between granules to capture internal cohesion and rigid-body behavior. The sinter bond strength evolves nonlinearly with ablation and aerodynamic loading. As the number of granules increases, forming hyperstatic structures with granular loops, the minimum spanning tree and depth-first search algorithms are employed to estimate the internal stress distribution of the sinter bond network. When the internal stress exceeds bond strength, the bond breaks, and the interaction transitions to Hertzian contact, allowing relative motion between granules. Parametric simulations using the new method reveal how internal structure influences the fragmentation cascade, supported by validation from the bilobate-shaped Fragment 109 of the Morávka meteoroid.

Posters

100 - ANOMALOUS COMET TAILS, IMPACT FROM METEOROIDS AND SOLAR ACTIVITY

Science Topic(s): Large impacts and Planetary Defence, Meteoroid Impact Physics

Guliyev Ayyub (Shamakhy Astrphysical Observatory (Azerbaijan))
co-authors: Guliyev Rustam, Kasimov Azi

The goal of the first part of the study is to study the directions of potential collisions between meteoroids and comets. The inclinations of 78 comets with anomalous tails were calculated in relation to 112 known meteoroid streams. In order to facilitate the calculations, the authors restricted themselves to cases where the MOID values of comets and streams did not exceed 0.01au. It was found that the distribution of I for long-period comets is characterized by a maximum near 1800. At such inclinations, the probability of forming an anomalous tail in collisions is high. The second part of the work analyzes the possible influence of solar activity (SA) on the formation of anomalous tails in some comets. Authors try to find out in which SA phases anomalous tails most often appear. For this purpose, the epochs of the formation of anomalous tails for 78 comets are compared with the phases (F) of SA in the corresponding periods. the value of F is normalized in such a way that the intervals of F correspond to equal periods of time. Summary N(F) is characterized by the mean and standard deviation of 5.32 and 1.20. The application of Student's t-distribution shows that it is uneven, which is due to the maximum (N= 7.4) in the F interval from 0.7 to 0.8. The confidence probability of the maximum number is greater than 0.95.

101 - Atmospheric behavior and internal structure of large meteoroids

Science Topic(s): Composition and Physical Properties, Meteor Physics and Chemistry

Jiri Borovicka (Astronomical Institute of the Czech Academy of Sciences)

The contribution presents the light curves of bright bolides associated with the entry of large meteoroids (>40 cm) and small asteroids. These include the pre-impact discovered bodies 2023 CX1, 2024 BX1, and 2024 XA1. The presented bolides encompass a range of meteorite types, namely ordinary and carbonaceous chondrites, along with an aubrite. In the majority of the examined cases, meteorites were also produced and recovered. When not affected by early fragmentation, the bolides exhibited fainter luminosities at altitudes exceeding approximately 65 km than would be predicted by standard equations. The potential causes of this phenomenon are discussed. Furthermore, the modeling of atmospheric fragmentation is used to study the distribution of strength inside the meteoroids. The internal structure of these asteroidal materials, which is difficult to study using other methods, is schematically visualized.

102 - Impact risk from a heliocentric dust ring on Venus orbit

Science Topic(s): Dust Particles and Clouds in the Solar System and Beyond

Ariane Courtot [early-career researcher] (ESA/ESTEC)
co-authors: Mark Millinger

Recently, a heliocentric dust ring on Venus orbit has been detected and some of its parameters have been evaluated (Leinert & Moster, 2007; Jones et al., 2013, 2017; Pokorny & Kuchner, 2019; Stenbord et al., 2021). This region of space gets crossed by spacecrafts using Venus as a gravity assist or studying Venus, Mercury or the Sun, so the impact risks it may poses to spacecrafts crossing this region of space have to be computed. To do this, we developed a model of the dust ring, from which the evolution of the ring over 2000 years was computed. It tends to spread out in width, with the smallest particles drifting the closest to the Sun. It also spreads out slightly in height. The number density in the ring is particularly high right near Venus orbit, then decreases sharply both in width and height. The amount of particles in the ring is then computed. From this, the impact flux is evaluated on Bepi-Colombo, which serves as an example of a spacecraft crossing the ring. The speed and direction of impacts are also computed. From these three indicators (number, speed and direction of impacts), a first assessment of the risk posed by the ring can be done: it does not seem to be a major threat. However, this study showed clearly the lack of data we have on the dust ring, and it is therefore highly necessary to keep monitoring it to gather more information.

103 - Solar System lottery: what were the chances?

Science Topic(s): Dynamical Evolution, Future Methods and Techniques

Sophie E. Deam [student] (Space Science and Technology Center, Curtin University, Australia)
co-authors: Hadrien Devillepoix

Calculating the impact probability between two objects orbiting the Sun is a classical problem in astronomy. Analytical techniques have been developed for decades, from Öpik formalism [1] to more robust techniques for varied orbits [2]. Numerical techniques are an alternative option and are commonly used in NEO monitoring and orbit propagation to assess impact risks such as NASA's sentry [3]. The appropriateness of any particular technique depends on the application, such as long vs short term assessment, single object or population wide calculations, or the uncertainties of the orbits being evaluated. Which method is most appropriate for the post-impact evaluation of an impacting orbit? I will present a comparison between probabilities evaluated using two techniques for fireballs on near-Earth orbits recorded by the Global Fireball Observatory. I aim to prompt a discussion around the strengths and weaknesses of each technique, and the considerations necessary when choosing one technique over the other. [1] Öpik, E. J. 1951, PRIAA, 54, 165 [2] Pokorný, P., & Vokrouhlický, D. 2013, Icar, 226, 682 [3] Roa, J., Farnocchia, D., & Chesley, S. R. 2021, AJ, 162, 277

104 - Estimating of the meteor parameters under various effects

Science Topic(s): Meteor Physics and Chemistry

Vladimir Efremov [early-career researcher] (Sadovsky Institute of Geosphere Dynamics RAS, Moscow, Russia)
co-authors: Olga Popova, Sadovsky Institute of Geosphere Dynamics RAS, Moscow, Russia, Anastasiia Bushmanova, Sadovsky Institute of Geosphere Dynamics RAS, Moscow, Russia, Anna Kartashova Institute of Astronomy RAS, Moscow, Russia

Small meteor parameters are estimated based on two different ablation models. Optical observations of the 2016 Perseid shower provided initial data to estimate the meteoroid parameters. Meteors weaker than -2^m were selected. The parameters (mass, size, density) estimated with the help of two different ablation models are compared. A number of model parameters are varied. The models, their results and uncertainty, and factors, which affect obtained results are discussed.

105 - Aqueous Processing on Asteroid Ryugu

Science Topic(s): Sample-Return Material and Meteorite Geochemistry

George Flynn (State University of New York - Plattsburgh)
co-authors: Paul Northrup

We analyzed sections from two aggregate grains by XRF and XAS, electron microprobe, and SEM-EDX, focusing on carbonate and apatite, each indicating fluid composition. Carbonate zoning shows ankerite cores, suggesting Fe metal buffered fO2 below the stability field of magnetite, allowing ankerite precipitation. After all initial Fe metal was oxidized, fO2 rose allowing magnetite precipitation. This lowered Fe2+, so carbonate switched to dolomite, entraining small magnetites. A Mg- and Mn-rim suggests dolomite growth stopped when Ca was depleted, allowing magnesite growth. Apatite shows an Mn-rich rim, suggesting both minerals formed from the same fluid(s), with fluid composition changing over time. Apatite has F<0.75 wt%) and negligible Cl, so the fluid had very low halogen to water. Mn is high in apatite. Mn-XAS confirms Mn is mostly Mn2+ in the Ca site of apatite. Increased F near the apatite and carbonate rims indicates the F content of the fluid evolved over time.

106 - Extracting Surface Temperature From Spectral Data at Martian Impact Craters

Science Topic(s): Impacts on Other Planets/Surfaces, Future Methods and Techniques

Michael Frazer [student] (Space Science and Technology Centre, Curtin University)
co-authors: Eriita Jones, Katarina Miljkovic, Mark McDonnell

Thermal infrared (TIR) observations of the martian surface, collected at λ ~ 13 µm, provide information about the temperature and physical characteristics (e.g. particle size and degree of cementation) of the top few tens of centimetres of the surface. This data is complimented by spectral observations of the surface in the visible and shortwave infrared, at λ ~ 0.4 – 4.0 µm, which provides information about the composition of the material. The spectral data is collected at a spatial resolution of 16 m/pixel, however the TIR data is only available at 100 m/pixel, preventing comparative studies of regions smaller than a few hundred metres including exposed rock out-crops, small impact craters, and potential landing and traverse sites for missions. Prior work has been completed which allows the temperature to be extracted from the spectral data by applying multi-sensor data fusion techniques and by finding solutions to thermal radiative transfer models. Here, we use machine learning to combine these two approaches and ‘predict’ the TIR data at λ ~ 13 µm based on the spectra between at λ ~ 0.4 – 4.0 µm, which will allow for the development of novel high-resolution TIR datasets. It demonstrates the strength of machine learning-based spectral analysis in planetary science, as well as an application of multisensor data fusion techniques.

107 - Dynamic Trajectory Fit for Space Debris Re-Entry: Insights from the Crew 5 Dragon Event

Science Topic(s): Human-generated Debris, Future Methods and Techniques

Bella Hatty [student] (Curtin University)
co-authors: Eleanor K. Sansom, Hadrien A. R. Devillepoix, Martin C. Towner, Trent Jansen- Sturgeon

Natural objects entering the Earth’s atmosphere is a subject of extensive research. Models range from basic straight-line deceleration to complex fragmentation and curved trajectories due to Earth’s rotation and gravity. Space debris re-entering from Low Earth Orbit (LEO) can be similarly modelled, but their long, shallow trajectories render some assumptions for natural objects invalid. Current models often oversimplify dynamics by neglecting lift and lateral velocity components, reducing accuracy in modelling the trajectories of re-entering debris. The Dynamic Trajectory Fit (DTF) method developed by Jansen-Sturgeon et al. (2020) removes the straight-line assumption by fitting differential equations of motion directly to the measured lines of sight, capturing full spatial and temporal information. We applied the DTF method to the 27 April 2023 re-entry of a Crew 5 Dragon trunk section, observed by Global Meteor Network (GMN) and Global Fireball Observatory (GFO) cameras over California. These networks, though not purpose-built for re-entries, incidentally capture such events and provide valuable observational data. Below altitudes of 200km, there is a global lack of monitoring capability which limits validation of predicted re-entry times and locations for re-entering debris. The DTF method, coupled with observations from meteor camera networks, can help fill this research gap and provide a foundation for including lift and lateral velocity components in future models.

108 - Meteor Orbit Characteristics Based on 2022–2023 Observations from Meteor Radar at KFU

Science Topic(s): Meteoroid Sources, Dust Particles and Clouds in the Solar System and Beyond

Sergey KALABANOV (Kazan Federal University, Institute of Physics)
co-authors: S.A. Kalabanov, D.V. Korotishkin , R.A. Ishmuratov, A.V. Izymchenko

The orbital structure of a meteoric complex in the vicinity of the Earth’s orbit is largely determined by the conditions under which it is observed from Earth. The antenna system of the new Kazan Meteor Radar (KMR) features an all-sky view directional diagram. This new design enhances the radar’s sensitivity, enabling the detection of approximately 6,000 particles per day. Initial surveys show that KMR captures a significant contribution from sources in the Northern Hemisphere, which supports primary online analysis software for meteor detection and positional determination parameters. This study presents data from meteor radar observations conducted during the 2022-2023 period. The observation conditions revealed several types of orbits: internal orbits with an aphelion distance of approximately 1 AU and a wide range of perihelion distances, and external orbits with a perihelion distance of approximately 1 AU and a wide range of aphelion distances. The majority of the observed orbits were nearly circular, with both Q ~ 1 AU and q ~ 1 AU. Three-dimensional maps of meteor stream distribution, along with the number of meteors in these streams, were constructed based on perihelion and aphelion distances, as well as orbital inclinations. The orbital parameters of the most significant meteoric streams identified are also presented.

109 - Analysis of pre-perihelion non-stationary activity of comet 12P/Pons–Brooks in 2023

Science Topic(s): Meteoroid Sources, Dust Particles and Clouds in the Solar System and Beyond

Gulchehra Kokhirova (Institute of Astrophysics, National Academy of Sciences of Tajikistan)
co-authors: Marek1 Husárik1, Firuza2 Rakhmatullaeva2, Oleksandra3 Ivanova3

Comet 12P/Pons–Brooks is a periodic comet with an orbital period of approximately 71 years. Because of the period duration, aphelion of 35.3 AU, and highly inclined orbit (74.2°), it classified as the Halley-type comet. The comet is considered the potential parent of the weak December κ Draconids meteor shower. We present the results of analysis of photometric and spectra observations of comet 12P at a heliocentric distance beyond 2.5 AU, before perihelion passage. Quasisynchronous observations were carried out from July to November 2023 using 0.61-m and 1.3-m telescopes Skalnaté Pleso Observatory (Astronomical Institute of the Slovak Academy of Sciences, IAU code 056), and 1-m telescope Zeiss-1000 Sanglokh International Astronomical Observatory (Institute of Astrophysics, National Academy of Sciences of Tajikistan, IAU code 193). Photometric observations were conducted using B, V, and R filters of the Johnsons-Cousins photometric system. During this period, the photometric data measured in the R filter such as the apparent (absolute) magnitudes and the Afρ(0°) values indicate several repeated outbursts in brightness and dust productivity occurred on around July 22, September 25, October 17-23, and significant outbrst was recorded on November 1-7. Comparision the dust production rate and the production rates of CN highlights that dust activity increased significantly as the comet approached the Sun, while gas activity exhibited more moderate changes.

110 - Dust productivity of comet C/2021 S3 (PANSTARRS) in 2024

Science Topic(s): Dust Particles and Clouds in the Solar System and Beyond, Influx of Interplanetary and Interstellar Material

Gulchehra Kokhirova (Institute of Astrophysics, National Academy of Sciences of Tajikistan)
co-authors: Firuza1 Rakhmatullaeva1

We present the results of photometric observations of comet C/2021 S3 PANSTARRS, which were performed during it post-perihelion period at the Sanglokh Observatory of the Institute of Astrophysics, National Academy of Sciences of Tajikistan. Monitoring has been carried out over 5 nights in June-July 2024 on the Zeiss-1000 telescope using the Johnson-Cousins broadband BVR filters. The processing of images was performed by Tycho software (https://www.tycho-tracker.com) using the Atlas Sky catalog (https://www.staratlaspro.com), the measurement aperture is selected taking into account the SNR. The measured magnitudes show an increase in the comet's brightness by about 1 mag from June to July, associated with a local dust emission. This is also indicated by the morphology of the comet's images and the dust productivity parameter. The comet was at a heliocentric distance of 2.2-2.7 AU and dust ejection was been still occurring under the influence of solar heating.

111 - Software calculation and visualization of secondary processing of meteor velocities and other parameters

Science Topic(s): Future Methods and Techniques

Iryna Kyrychenko [student] (Kharkiv National University of Radio Electronics)
co-authors: Kyrychenko I., Kolomiyets S., Kysil L.

Receiving a scattered signal from the Kharkov MARS meteor radar allows us to determine, in addition to the velocity, the coordinates of the meteor's radiant (in the presence of three reflected points), which fully provides the researcher with information for determining orbits and their parameters using a secondary processing algorithm. This allows us to solve the problem of the meteor's orbit structure. Primary measurements of the range, extreme positions and time delay values, as well as velocities and orbit calculations were carried out in a fully automated mode. The algorithm for secondary processing of meteor velocities and orbit parameters is a sequence of steps aimed at improving the accuracy of measurements, calculations and visualization of the orbital characteristics of meteors after the primary data collection, which allows us to more accurately determine and visualize the distribution of meteor bodies in the Solar System and can be added to international catalogs of meteor orbits, which is important for studying the evolution of near-Earth space and monitoring potentially dangerous meteoroids. The application combines scientific and technological components, as it is built on modern web technologies such as Go, Deno and ESBuild. The development of the algorithm is part of the open source trend, which give opportunities for scientists and developers. This ensures transparency of research, allows for improvements and the creation of alternative solutions.

112 - Meteorite Parent Bodies in the Near-Earth Object Population

Science Topic(s): Meteoroid Sources

Nicholas Moskovitz (Lowell Observatory)

Telescopic surveys for near-Earth objects (NEOs) have become increasingly efficient at discovering bodies that are decameter scale and smaller. Objects at this small end of the NEO size frequency distribution are our best available analogs to meteorite parent bodies in space, and thus provide a means to improve understanding of the connections between asteroids and meteorites. For example, the diversity of asteroid compositions in space, when compared to the distribution of meteorite types that survive to the ground, can directly inform selection biases imposed by the atmosphere. However, telescopic follow-up of these small NEOs is challenging due to short observing windows, faint apparent magnitudes, and rapid non-sidereal motion on sky. I will present on the state of knowledge regarding the distribution of spectroscopically-derived compositions of NEOs in the decameter size regime. Recent and ongoing work suggests that the reflectance spectra of small NEOs differ from that of their larger counterparts. This result could indicate one or more of the following phenomena influences spectral properties: (1) size-dependent compositional variation in the NEO population, (2) a size-dependent change in NEO surface properties such as regolith grain size, and (3) discovery bias in favor of low perihelion NEOs where thermal alteration of surfaces may be more pronounced. Evidence for these possibilities along with implications for the asteroid-meteorite connection will be presented.

113 - Fusion crust: from the initial meteoroid matter to the observation spectrum

Science Topic(s): Composition and Physical Properties

Evgeniya V. Petrova (Ural Federal University, Ekaterinburg, Russia)
co-authors: Anna P. Kartashova (Institute of Astronomy RAS, Moscow, Russia), Victor I. Grokhovsky (Ural Federal University, Ekaterinburg, Russia)

The fragmentation, ablation and significant loss of mass occur during the meteoroid pass through the Earth’s atmosphere. There a combined action of melting and shearing takes place, so a fusion crust is forming on the surface of the fragments. It combined a subsurface layer of heated matter and an outer layer consisting of remaining melted meteoroid substance. Comparative studies of the bulk interior and the fusion crust of meteorites Chelyabinsk LL5, Ozerki L6, Kemer L4, and Calama 009 L6 were carried out. It was shown that the amount of iron-containing phases such as Ca-rich clinopyroxene, troilite, orthopyroxene and Fe(Ni, Co) phase are reduced in the fusion crust. Apart from that, new phases such as magnesioferrite, are formed in the fusion crust (M.I. Oshtrakh et al., 2023; E.V. Petrova et al., 2024). Besides, globules enriched in platinum group elements were found in the fusion crust of the Chelyabinsk meteorite (V.V. Sharygin et al., 2019). While, in the spectra recorded during the fall of meteoroids, lines corresponding to Mg and Na, K, Li, Mn, Cr, and Ti are observed (P. Spurný et al., 2024). At the ablation modeling experiments using a plasma torch with the meteoroids of chondritic composition, the spectral lines of Cu, Fe, N, and O were captured (Lei Wang et al., 2024). All this tends to confirm that elements heavier than Ni and Co can be concentrated in the fusion crust of chondrites. This research was funded by RSF (project № 24-27-00392).

114 - Global Meteor Network - Australia

Science Topic(s): Meteoroid Sources

Derek Poulton (Astronomical Society of Victoria)

The Global Meteor Network (GMN) was formed in 2017. The concept is a citizen science project using a raspberry pi computer and digital Sony IMX291 camera, for under $500. RMS software was developed to allow data to be processed and made available in the public domain. The aim of GMN is to publish meteor observations from across the world every morning; observe meteor showers and determine radiants, flux, mass and orbits; and detect fireballs and strewn zone for associated meteorite falls. In Australia, the first cameras appeared in about 2020. GMN has expanded rapidly and there are currently 120 cameras across all states and territories. The GMN has been successful in describing several new meteor radiants. Fireballs are regularly observed and sometimes result in meteorite searches. The GMN network in New Zealand successfully detected a fireball and recovered a meteorite in South Island. In Victoria we have detected several fireballs, and conducted two searches – but no rocks yet. GMN has a well-planned and coordinated outreach program. Perth Observatory, in conjunction with GMN, deployed a number of cameras in West Australia to schools and libraries. This poster describes current status, observations and future directions of the GMN network in Australia.

115 - A New Fireball Detection Pipeline via Machine Learning and Supercomputing

Science Topic(s): Future Methods and Techniques

Jun Christian Saniel (Curtin University)
co-authors: Hadrien Devillepoix, Eleanor Sansom, Martin Cupak, Tom Gedeon, Martin Towner

This work introduces a new fireball detection pipeline developed for the Desert Fireball Network (DFN), designed to process archived all-sky images using modern machine learning and computer vision techniques. Unlike the DFN's existing detection system onboard their observatories, which emphasises efficiency due to hardware constraints, this pipeline is optimised for performance and accuracy on high-performance computing infrastructure, particularly the Setonix supercomputer at the Pawsey Supercomputing Research Centre. The system performs advanced image differencing with sub-pixel alignment to suppress static background elements and stellar misalignment artefacts. Images are then tiled with 50% overlap to preserve streak continuity across tile borders. YOLOv8, a deep learning object detector, is trained on known DFN events to identify fireball streaks in image tiles. A post-processing stage performs blob detection and robust line fitting to verify trajectory validity and filter out noise, duplicates, and satellite trails. Applied to archived data from January 2015, the system successfully recovered all 38 known fireballs and identified an additional 243 previously overlooked events. This scalable pipeline enables retrospective analysis of over a decade of DFN data, promising substantial improvements in fireball research.

116 - WMPGang SkyShield: An Interactive Web App for Near-Earth Object and Meteoroid Risk Visualization

Science Topic(s): Meteoroid Sources, Large impacts and Planetary Defence

Maximilian Vovk [student] (Western University)
co-authors: Dakota Cecil, Ian Chow, Simon Van Schuylenbergh

The WMPGang team developed SkyShield, an interactive web app that won the best use of science award for the 2024 NASA International Space Apps Challenge. The app visualizes Near-Earth Object (NEO) threats and meteoroid hazards to satellites, addressing the often-overlooked risk posed by meteoroids to satellites. Using NEO data, meteor stream distributions, and the sporadic meteoroid complex, SkyShield presents a 3D orrery of the solar system where users can explore celestial objects, toggle data layers, and simulate orbital motion. Built with JavaScript, Three.js, and Python for data preprocessing, SkyShield displays the orbits of planets and dwarf planets, 1,669 NEOs, 34 meteor showers, and 107 individual shower streams. Users can filter NEOs by risk parameters and track objects in real-time. This tool enhances awareness of space hazards and provides insights for satellite protection. SkyShield demonstrates how interactive visualization can improve scientific engagement and serve as a valuable educational tool for teaching orbital dynamics and space hazards.

117 - The relationship between bolide flight parameters and infrasound detection rates

Science Topic(s):

Miro Ronac Giannone (Sandia National Laboratories)
co-authors: Miro Ronac Giannone, Elizabeth A. Silber, and Vedant Sawal

118 - Computational framework for classifying bolide fragmentation dynamics

Science Topic(s):

Elizabeth A. Silber (Sandia National Laboratories)
co-authors: Elizabeth A. Silber, Vedant Sawal

119 - Entry geometry effects on infrasound detection of meteoroids and space debris

Science Topic(s):

Elizabeth A. Silber (Sandia National Laboratories)
co-authors: Elizabeth A. Silber

(Total: 89)