bluuebunny/crossref_metadata_2025 huggingface dataset:
 How earlier LSST would have discovered currently known long-period and hyperbolic comets?
Authors: Inno Laura , Bertini Ivano , Fulle Marco , Mazzotta Epifani Elena , Della Corte Vincenzo , Piccirillo Alice Maria , Lacerda Pedro , Scuderi Margherita , Vanzanella Antonio , Ferone Alessio , Grappasonni Chiara , Sindoni Giuseppe , Ammanito Eleonora , Rotundi Alessandra
Published: July 2024

Comets originating from the Oort Cloud are a rare and elusive group within our solar system, making them difficult to detect. However, these comets are some of the most pristine objects we can observe, offering vital insights into the formation of planetary systems, and thus, they are the subject of extensive scientific research and missions.The Legacy Survey of Space and Time (LSST), set to begin operations at the Vera C. Rubin Observatory in 2025, is anticipated to significantly enhance our ability to detect these comets. By regularly monitoring the Southern sky to a depth of magnitude 24 with high precision, the LSST will greatly improve our comet detection capabilities. However, predicting the future detection rates of the LSST is challenging due to our limited understanding of the underlying comet population. Previous identifications have been made by various surveys or individual observers, each with unknown selection biases.In this talk, we will explore an alternative method to estimate the LSST's performance by analyzing how early known comets on long-period or hyperbolic orbits would have been discovered if an LSST-like survey had been operational ten years prior to their perihelion. This approach cannot be used to make quantitative predictions for future incoming objects,  but it still shows that LSST can potentially increase the discovery rate of long-period and hyperbolic comets by at least five times. We will present our findings, discuss the limitations of the method, and share the insights gained from this exercise. 
Promoting Inclusive Participation at the Europlanet Science Conference: Strategies for Enhanced Accessibility
Authors: Calders Stijn , Piccialli Arianna
Published: July 2024

The Europlanet Science Conference (EPSC) is a cornerstone event that shapes the future of planetary sciences. Ensuring accessibility for researchers with disabilities is not just a matter of compliance, but a fundamental driver of scientific innovation and excellence. Diverse perspectives, including those from researchers with disabilities, enrich scientific discourse, foster creativity, and lead to more comprehensive and impactful discoveries. This abstract highlights the critical importance of inclusivity and presents practical strategies to enhance accessibility at EPSC.Full participation of researchers with disabilities ensures that the scientific community benefits from the broadest range of talents and insights. Addressing current barriers, such as physical obstacles, inadequate assistive technologies, and inaccessible materials, is essential to achieving this goal. Proposed solutions include selecting fully accessible venues, providing materials in multiple formats, offering real-time captioning and sign language interpretation, utilizing technology to support remote participation, and training staff in best practices for accessibility. Additionally, establishing clear policies and feedback mechanisms can help maintain a welcoming and inclusive environment.By implementing these strategies, EPSC can set a standard for accessibility in scientific conferences, demonstrating a commitment to inclusivity that benefits the entire planetary science community. Ensuring that all researchers can engage fully and contribute their unique perspectives will lead to richer scientific dialogue and more robust advancements in the field.
Bioverse: Probing the Habitable Zone Inner Edge Discontinuity and the Origins of Life
Authors: Schlecker Martin , Apai Daniel , Lichtenberg Tim , Bergsten Galen , Salvador Arnaud , Hardegree-Ullman Kevin , Affholder Antonin , Ranjan Sukrit , Ferriere Regis , Mazevet Stephane , Heng Kevin
Published: July 2024

Studying planetary habitability has become a major emerging research area, with critical implications for future exoplanet exploration and ambitious ground- and space-based telescopes. Efforts to design and optimize these missions have been focusing on maximizing the planet yield – the number of exoplanets a survey will be able to characterize – which is not necessarily equivalent to science return. We present Bioverse, a framework to quantify the diagnostic power of nextgeneration exoplanet surveys Bioverse allows to assess the detectability of population-level trends injected in simulated planet populations. Here, we apply Bioverse to explore the requirements for a mission to probe and characterize the inner edge of the habitable zone. We show that, through probing a discontinuity in the distribution of planetary radii and bulk densities caused by the runaway greenhouse transition, the PLATO mission will likely be able to constrain this demographic feature. This will constitute the first empirical test of the habitable zone concept.We further use Bioverse to demonstrate how contextual information about a planet with a biosignature detection, such as its orbit or properties of its host star, lend or take away credibility from competing models of abiogenesis. We demonstrate that planet sample sizes ≥100 enable a strong test of a predicted correlation between past received nearultraviolet flux and the occurrence of biosignatures in the cyanosulfidic scenario for the origin of life.Probabilistic assessments that take into account the population context will be critical for an effective search for extraterrestrial life in the Universe and to constrain the origin of life.Figure 1. Detection of the Habitable Zone Inner Edge Discontinuity. We fit a population-level runaway greenhouse model (red posterior draws) to simulated radius measurements and test this hypothesis against the null hypothesis of an irradiation-independent distribution. In a large (N = 500) planet sample, the discontinuity is detected with high confidence.References:Bixel, A., & Apai, D. 2021, The Astronomical Journal, 161, 228, doi: 10.3847/1538-3881/abe042Dorn, C., & Lichtenberg, T. 2021, ApJL, 922, L4, doi: 10.3847/2041-8213/ac33afRanjan, S., Wordsworth, R., & Sasselov, D. D. 2017, Astrobiology, 17, 687, doi: 10.1089/ast.2016.1596Schlecker, M., Apai, D., Lichtenberg, T., et al., The Planetary Journal, in press. [arXiv:2309.04518]Turbet, M., Bolmont, E., Chaverot, G., et al. 2021, Nature, 598, 276, doi: 10.1038/s41586-021-03873-w 
The Massalia asteroid family as the origin of ordinary L chondrites
Authors: Marsset Michaël , Vernazza Pierre , Brož Miroslav , Thomas Cristina , DeMeo Francesca , Burt Brian , Binzel Richard , Reddy Vishnu , McGraw Allison , Avdellidou Chrysa , Carry Benoit , Slivan Stephen , Polishook David
Published: July 2024

Studies of micrometeorites in mid-Ordovician limestones and Earth’s impact craters indicate that our planet witnessed a massive infall of ordinary L chondrite material ~466 million years (My) ago (Heck et al. 2017, Schmieder & Kring 2020, Kenkmann 2021) that may have been at the origin of the first major mass extinction event (Schmitz et al. 2019). The breakup of a large asteroid in the main belt is the likely cause of this massive infall. In modern times, material originating from this breakup still dominates meteorite falls (>20% of all falls) (Swindle et al. 2014). We will present spectroscopic observations and dynamical evidence that the Massalia collisional family is the only plausible source of this catastrophic event and of the most abundant class of meteorites falling on Earth today.
Dust dynamics modelling on the main-belt comet 324P/La Sagra 
Authors: Mastropietro Maria , Kim Yoonyoung , Agarwal Jessica
Published: July 2024

Main-belt comets (MBCs) are comet-asteroid transition objects, orbiting in the main asteroid belt. They exhibit cometary mass loss due to the sublimation of volatile ices [1]. During their active phase, MBCs eject both small and large particles. Large particles that are less affected by solar radiation pressure tend to stay closer to the nucleus of the comet and do not disperse as quickly into space as the smaller particles. The size of the large particles can inform us about the strength of the gas drag and the rate of ice sublimation. The study of ice content in MBCs allows us to constrain the distribution of volatiles in the early solar system and the formation and subsequent evolution of planetesimals.   

The presence of smaller particles complicates the measurement of larger particles due to the higher scattering cross-section of the former. One of the key observational techniques to measure the size of large particles involves analyzing the brightness profile of dust trails produced during inactive phase, when MBCs do not produce new dust and gas, allowing clearer observation of previously ejected large particles, if present.   

The MBC 324P/La Sagra has been observed to emit dust during three subsequent perihelion passages in 2010, 2015 and 2021 [2][3]. It is peculiar for developing a gap between the nucleus and the tail after the cease of its activity [4][5]. From the size of the gap, it is possible to constrain the size of the largest particles.   

Utilizing the syndyne-synchrone modeling code, we analyzed a coadded image of 324P/La Sagra that shows a faint trail on 31 December 2011, a period during which the MBC was inactive at true anomaly of 117°. The study revealed large dust particle sizes ranging from 0.2 mm to 0.8 mm over a three-month period. Further, we compared the synchrone ages with the activity profile of 324P/La Sagra to establish a temporal correlation between the particle ejection events and the historical activity phases of the MBC. 
 

References: 

[1] Hsieh, H. H. and D. Jewitt (2006) "A Population of Comets in the Main Asteroid Belt", Sci, 312, 561 

[2] Hsieh, H. H. and S. S. Sheppard (2015) "The reactivation of main-belt Comet 324P/La Sagra (P/2010 R2)", MNRAS, 454, L81 

[3] Mastropietro, M., et al. (2022) "Activity of the Main-Belt Comet 324P/La Sagra", EPSC, EPSC2022-1211 

[4] Hsieh, H. H. (2014) "The nucleus of main-belt Comet P/2010 R2 (La Sagra)", Icar, 243, 16 

[5] Snodgrass, C., et al. (2018) "The Castalia mission to Main Belt Comet 133P/Elst-Pizarro", AdSpR, 62, 1947 
Characteristics and Changes in Ammonia Abundance Features in Jupiter’s Upper Troposphere 2022-2023
Authors: Hill Steven , Irwin Patrick , Alexander Charlotte , Rogers John
Published: July 2024

Amateur observers (Hill et al., 2024) have shown that filter-averaged measurements of the reflectance of Jupiter in molecular absorption bands of ammonia and methane can be made with modest-sized telescopes and reduced to yield spatial maps of ammonia. We now create an empirical limb correction for the ammonia abundance and effective cloud-top pressure and assemble sets of synoptic maps with partial or complete longitude coverage taken in moderately close temporal proximity (fewer than 10 Jupiter days). We then examine the maps to evaluate the characteristics and changes seen in localized ammonia enhancements and gradients in the context of effective cloud-top pressure and visual features. The ammonia depletion associated with the Great Red Spot (GRS) and the enhancements in the NEZ show significant contrast and are the focus of the study. The GRS region shows generally persistent characteristics over the period of observation, including a small southward offset of the depleted regions from the visual centroid of the GRS. The NEZ enhancements and their relationship to visual features such as plumes and North Equatorial Dark Features (NEDFs) are presented along with changes seen on timescales of days to weeks. This work demonstrates the utility of frequent observations in following the evolution of the Jovian ammonia distribution.
Temporal variability of thermal-cycling induced fracturing in chondrites
Authors: Latsia Nicol , Borg Johan , Kaufmann Erika , Suhonen Heikki , Tsirvoulis Georgios , Granvik Mikael , Hagermann Axel
Published: July 2024

Thermal fatigue is produced by diurnal and/or annual variations of the surface temperature on asteroids and its efficiency depends on the heliocentric distance, the rotation period, and the thermal inertia of the asteroid’s surface. A fundamental assumption of previous studies [1,2], is that thermal fatigue remains effective over thousands, or even millions, of thermal cycles. However, the Kaiser effect, extensively studied in the field of fracture mechanics on terrestrial rocks, states that fracturing on materials ceases when previously exerted load levels are not exceeded [3]. The thermal expansion coefficient of each mineral at specific temperature changes can be translated into different mechanical loads resulting from thermal fatigue.We aim to observe the time-resolved crack propagation induced by thermal stresses over subsequent thermal load cycles in meteorites – acting as asteroid analogues – in order to understand the role of thermal fatigue in eroding asteroid surfaces using non-destructive methods. We investigate CV, CM, and, for comparison, LL chondrites to examine the behaviour of thermal fatigue on different petrographic types of meteorites. The samples are subjected to a minimum of 100 cycles at ΔT=210K as a typical temperature variation of C-type NEAs is 200K [2]. To identify the spatial occurrence of pre-existing and propagating cracks, the samples have been scanned using X-ray μCT. If the Kaiser effect is applicable, we expect to see the effects of thermal fatigue wane after a few thermal cycles, suggesting that other mechanisms, such as chemical alteration, are contributing to the breakdown process of asteroids.[1] Delbo M. et al. 2014. Nature 508(7495) 233-236. [2] Molaro J.L. et al. 2015. JGR Planets 120(2) 255-277. [3] Kaiser J. 1950. A study of acoustic phenomena in tensile heat (PhD Thesis).
The response of the Venusian upper atmosphere during the passage of interplanetary coronal mass ejections
Authors: Rout Diptiranjan , Thampi Smitha , Miyoshi Yoshizumi , Pant Tarun , Bhardwaj Anil
Published: July 2024

The study explores the dynamic interaction between Interplanetary coronal mass ejections (ICMEs) and the induced magnetosphere of Venus, utilizing measurements from the Venus Express (VEX) mission. Over the period 2006-2013, we analyzed 16 ICME events, noting peak magnetic field strengths at the ionopause around 100 nT. Our investigation comprehensively examines the altitude of the inbound bow shock and ionopause during these ICME passages. The ionosphere is found to be highly magnetized due to the very high magnetic pressure of the induced magnetosphere.  Remarkably, the altitude of the ionopause is found to be significantly compressed as compared to the previous quiet day due to the increased solar wind dynamic pressure. Intriguingly, the bow shock position exhibited minimal deviations compared to typical quiet days, underscoring that, during ICME events, the ionopause location is more responsive to solar wind pressure fluctuations than the bow shock location. Additionally, we observed a notable increase in heavy-ion density near and above the ionopause compared to quiet days. This substantial increase implies that ICMEs can induce atmospheric loss in Venus’s atmosphere and also cause a significant reduction in the ionopause location.
Sunward oxygen ion fluxes and the magnetic field topology at Mars from hybrid simulations and observations
Authors: Dubinin Eduard , Modolo Ronan , Fraenz Markus , Paetzold Martin
Published: July 2024

It is commonly believed that because of the direct solar wind interaction with the Martian atmosphere/ionosphere, the planet could have lost a significant part of its atmosphere. Closed field lines of the crustal magnetic field can weaken a transport of the ionospheric ions to the tail. Reconnection of the interplanetary magnetic field lines draping around Mars and the crustal magnetic field can also lead to a presense of sunward fluxes of planetary ions that might affect the total ion loss. The LatHyS (LATMOS Hybrid Simulation) three-dimensional multispecies hybrid model is used here to characterize sunward fluxes of O+ and O2+ions and the magnetic field topology at Mars. It is shown that although reconnection between the interplanetary magnetic field (IMF) and the crustal magnetic fields strongly modifies the field topology, then sunward ion fluxes are rather small and do not significantly change the total ion loss. The results are compared with the MAVEN data.
Exploring Synergies between Twinkle and Ariel: a Pilot Study
Authors: Bocchieri Andrea , Booth Luke , Mugnai Lorenzo V.
Published: July 2024

Twinkle and Ariel, set to launch in 2025 and 2029 respectively, will conduct the first large-scale homogeneous spectroscopic surveys of hundreds of exoplanet atmospheres. This will fully transition the field to an era of population-level atmospheric characterization. In this pilot study, we explore synergies between the two missions by focusing on a select subset of 'cool' planets well-suited for observation by both telescopes.Using representative noise levels, we compute the number of visits needed, simulate and retrieve observed transmission spectra assuming gaseous, H2/He-dominated atmospheres. We will show that for all targets, atmospheric parameters are generally retrieved within 1-sigma of input values, with Ariel achieving tighter constraints. We will demonstrate exploitable synergies between Twinkle and Ariel for this 'cool' planet sample, with Twinkle potentially providing a vantage point to plan Ariel observations. As the missions' target lists take shape, we encourage further investigation by both consortium communities to fully map the synergy potential as the launch dates approach.
The Moon is an exciting object for space plasma physics: the main science questions
Authors: Barabash Stas
Published: July 2024

Traditionally the Moon is considered “boring” by space plasma physicists. Indeed, no dense atmosphere/ionosphere, no large scale magnetic field, and the solar wind absorption by non-conductive surface make this body an outcast among “exciting” objects being the primary interest for space plasma physics. However, lunar exploration for the last 20 – 25 years revealed a completely different picture of our only satellite. The Moon is non-magnetized body but possesses magnetic anomalies, localized (mostly on the far side) magnetic field structures of
Mauve: a UV-Vis satellite dedicated to monitor stellar activity and variability
Authors: Majidi Fatemeh Zahra , Bradley Lawrence , Ma Sushuang , Saba Arianna , Tinetti Giovanna , Stotesbury Ian , Edwards Billy , Savini Giorgio , Favata Fabio , Tessenyi Marcell , Wilcock Benjamin John
Published: July 2024

Mauve is a satellite equipped with a 13-cm telescope and a UV-Visible spectrometer (with anoperative wavelength range of 200-700 nm) conceived to measure stellar magnetic activity andvariability. The science program will be delivered via a multi-year collaborative survey program,with thousands of hours each year available for long baseline observations of hundreds of stars,unlocking a significant time domain astronomy opportunity. Mauve’s mission lifetime is 3 yearswith the ambition of 5 years, and will cover a broad field of regard (–46.4 to 31.8 degrees in ICRS)during this period. This facility was conceived to support pilot studies and new ideas in science and is fully dedicatedto time-domain astronomy. The main surveys to be executed by Mauve are monitoring of- Flare stars (ﬂares, depending on their energy and frequency, may change the chemistry of planetary atmospheres, power prebiotic chemistry, produce surface biosignatures, or deprive exoplanets of their atmospheres totally)- Herbig Ae/Be stars (which host protoplanetary disks and few of them are young exoplanet hosts/candidate exoplanet hosts)- Confirmed exoplanet hosts,- Contact binary variables (RS CVn variables, symbiotic stars, Algol-type stars, etc.), with several of them hosting exoplanets, such as AF Lep, the recently discovered benchmark system to be studied for exoplanet atmosphere characterisation for its unique features.Besides these major science themes, the spectrometer’s data can be utilized to support and complement existing and upcoming facilities as a pathfinder, or conduct simultaneous/follow-up observations.
The Negative Ions at the Lunar Surface (NILS) instrument on Chang’E-6: the instrument, objectives and first results
Authors: Canu-Blot Romain , Wieser Martin , Barabash Stas , Kérényi Maté , Xiao-Dong Wang , Melville Neil
Published: July 2024

Mission description

The Negative Ions at the Lunar Surface (NILS) instrument (Fig. 1) is the first instrument to measure negative ions directly on the lunar surface. Launched aboard the Chinese Chang’E-6 sample-return mission on May 3, 2024, the instrument will land on the lunar far-side (South Pole-Aitken basin) in early June 2024. During the surface phase of the lander, the NILS instrument will be active, measuring negative ion and electron fluxes from the lunar surface.
Scientific objectives

When the solar wind interacts with the lunar surface, a portion of it is reflected back instead of being absorbed. Previous studies have provided evidence of neutral hydrogen atoms [1] and solar wind protons [2] being reflected from the surface. However, to date, no measurements of negative ions have been conducted. It remains unclear whether a significant population of negative ions exists near the lunar surface. The NILS instrument, the first-ever dedicated negative ion instrument flown beyond the Earth, will address this gap by performing in-situ measurements directly on the lunar surface.
Instrument description

The NILS instrument is a 9th generation instrument of the SWIM family [3]. NILS uses a surface-interaction based time-of-flight system combined with an electrostatic analyzer and an electrostatic elevation scanning system to measure the direction-, energy-, and mass-resolved negative ion flux on the surface. A electromagnetic electron suppression system allows to switch between negative ion and electron measurements. NILS can separate the main solar wind components as well as negative sputtered oxygen ions and heavier species. Key performance parameters are shown in Table 1.Table 1: Instrument performancesFigure 1: NILS flight modelAt the Europlanet Science Congress 2024, we present and interpret the first data obtained and discuss the implications of the observed negative ion flux on the lunar near-surface plasma environment.
References

[1] M. Wieser, S. Barabash, Y. Futaana, M. Holmström, A. Bhardwaj, R. Sridharan, M. B. Dhanya, A. Schaufelberger, P. Wurz, and K. Asamura. First observation of a mini-magnetosphere above a lunar magnetic anomaly using energetic neutral atoms. Geophys. Res. Lett., 37(5), 03 2010.[2] Y. Saito, S. Yokota, T. Tanaka, K. Asamura, M. N. Nishino, M. Fujimoto, H. Tsunakawa, H. Shibuya, M. Matsushima, H. Shimizu, F. Takahashi, T. Mukai, and T. Terasawa. Solar wind proton reflection at the lunar surface: Low energy ion measurement by map-pace onboard selene (kaguya). Geophys. Res. Lett., 35, 12 2008.[3] M. Wieser and S. Barabash. A family for miniature, easily reconfigurable particle sensors for space plasma measurements. Journal of Geophysical Research: Space Physics, 2
Within the Surveys: Spins of asteroids derived from Gaia DR3 and ATLAS photometry
Authors: Ďurech Josef , Hanuš Josef
Published: July 2024

Large surveys are invaluable sources of asteroid photometry. If there are enough data points with sufficient photometric accuracy, this sparse-in-time photometry can be used for asteroid shape and spin-state reconstruction with the light curve inversion method [1], [2].We will present our results obtained by processing asteroid photometry from Gaia DR3 [3] and ATLAS [4]. We have derived convex shape models and spin states for about 15,000 asteroids. The distribution of asteroid spins across the main belt and in asteroid families is size-dependent and clearly shows that the rotation axes of asteroids are affected by the thermal YORP effect, which then affects the semimajor drift due to the Yarkovsky effect.Acknowledgments: This work was supported by the grant 23-04946S of the Czech Science Foundation.References: [1] Kaasalainen et al. (2001), Icarus 153, 37. [2] Kaasalainen (2004), A&A 422, L39. [3] Tanga et al. (2023), A&A 674, A12. [4] Tonry et al. (2018), PASP 130, 064505.
Gravity Wave-Induced Ionospheric Irregularities in the Martian Atmosphere
Authors: Tian Rong , Jiang Chunhua , Sánchez‐Cano Beatriz
Published: July 2024

For the past few decades, it has demonstrated that gravity waves (GWs) and neutral winds can drive ionospheric irregularities on Earth. Still, as far as we know, the formation of ionospheric irregularity on Mars due to GWs has not been well studied. In this study, we use data from NASA's Mars Atmosphere and Volatile Evolution (MAVEN) mission to show evidence of an irregularity event in the Martian ionosphere, which is potentially seeded by the break of GWs (GWB). The statistical findings indicate that the observed ratio of GWB-related irregularity events varies from ~0.25 to 0.57 in each year, and the overall correlation for 2015 to 2020 is ~0.37. Numerical simulations provide further insight into the processes behind irregularities formation, which employs neutral wind shear as a source of perturbation in the context of the GWB. The simulations yield results fundamentally aligned with the observed characteristics of ionospheric irregularities observed in the 2018 event by considering the wind shear as the disturbance source. This study provides supplementary insights into the perturbation sources involved in shaping irregularities within the Martian ionosphere and presents valuable information about the coupling between the Martian ionosphere and the lower atmosphere.
The recovery of the Matera H5 ordinary chondrite thanks to the observations of the PRISMA fireball network
Authors: Barghini Dario , Carbognani Albino , Gardiol Daniele , Bertocco Sara , Di Carlo Matteo , Di Martino Mario , Falco Carmelo , Fenucci Marco , Morelli Marco , Pratesi Giovanni , Riva Walter , Salerno Raffaele , Stirpe Giovanna Maria , Volpicelli Cosimo Antonio ,   PRISMA team
Published: July 2024

On 14/02/2023 at 17:68:29 UT, three all-sky cameras of the PRISMA network detected a bright bolide (IT20230214) over the regions of Puglia and Basilicata in Southern Italy. The bolide traversed the atmosphere for about 5.3 s, with an entry speed of 16.3 ± 0.1 km/s and at an inclination angle of 56.7° ± 0.3°, reaching a minimum absolute magnitude of -11. Projected on the ground, its trajectory began SW of Bari and ended NE of Matera. From the data collected by the PRISMA network, it was possible to fully characterize the meteoroid, which was determined to have a pre-atmospheric mass of 5 – 21 kg, corresponding to a size of 15 – 24 cm. Its pre-atmospheric orbit was determined to be of asteroidal origin, having a moderate eccentricity of 0.54 ± 0.02, an inclination on the ecliptic plane of 14.5° ± 0.2° and a semi-major axis of 2.10 ± 0.07 AU, with a Tisserand’s parameter of 3.51 ± 0.08. According to a photo-dynamic model, simultaneously fitting for the speed and magnitude data, the residual meteorite mass was determined to be 0.10 ± 0.04 kg (4.4 ± 0.7 cm of size). The area of fall of meteorites was estimated to be located north of Matera, in the Basilicata region. In this contribution, we discuss the analysis of the IT20230214 bolide and, in particular, the finding of the Matera meteorite on 17/03/2023, reported by the brothers Mr. Gianfranco and Pino Losignore in Contrada Rondinelle, in the municipality of Matera. With a total recovered mass of 117.5 g, the Matera meteorite was classified as an H5 ordinary chondrite.
The ExoClock project for the Ariel space mission- 5 years of continuous operation
Authors: Kokori Anastasia
Published: July 2024

The ExoClock project - www.exoclock.space – aims to monitor regularly transiting exoplanets for the Ariel space mission, using small- and medium-scale telescopes. The project launched in EPSC 2019 and in EPSC 2024  we celebrate five years of continuous operation. ExoClock is part of the ephemerides working group of ESA's Ariel space mission and its main scope is to maximise the mission’s efficiency. In this effort, our team has been actively collaborating with both professional and amateur astronomers coming from various countries around the world. Participants contribute with observations of exoplanets by using a wide range of telescopes, from backyard ones to large facilities own by organisations and universities. Apart from he science goal, our efforts include public engagement with science. In order to increase participation and enable/ facilitate research, we have created educational and user friendly tools while we have initiated / developed also dedicated projects for completely inexperienced people such as citizen scientists and school students.This presentation will describe how collaborative and open science can be used to advance exoplanet research though projects such as ExoClock. More specifically, I will talk about the organisation of the ExoClock project and the main tools that are used to achieve an effective pro-am collaboration. I will also present the status of the project and the results of the publications we have produced so far. The ExoClock network currently consists of more than 1400 participants, including professionals, amateur astronomers (75%), university students but also some citizen scientists. The talk will end with lessons learned from 5 years of operation and future plans. 
Physics Informed Neural Networks as addition to classical Precise Orbit Determination
Authors: Dallinger Fabian , Aigner Benedikt , Andert Thomas , Pätzold Martin
Published: July 2024

AbstractIn recent years, the integration of artificial intelligence (AI), especially machine learning (ML), has found entrance in various fields, including industry, medicine, self-driving cars and daily life. However, the application of ML tools in space science is still in its early stages and holds the potential to complement traditional methods. This study investigates the effectiveness of machine learning algorithms, with a focus on Physics Informed Neural Networks (PINNs) to expand or support the classical methods in orbit propagation and determination.PINNs were first introduced by Raissi et al. [1] and offer a promising avenue due to their unique ability to incorporate the governing differential equations of the system into the learning process, thereby imposing a physical constraint on the Networks predictions. This constraint enables effective training with sparse data, bypassing the need for large datasets typical for traditional Neural Network approaches. In addition, PINNs allow for the determination of unknown or poorly known parameters within the differential equation - a capability absent in conventional “Black-Box” Neural Networks.To demonstrate the usefulness of PINNs, we first present a case study on simulated data within the framework of the AI4POD (Artificial Intelligence for Precise Orbit Determination) software tool of RSOs in the low earth orbit. A similar approach using Physics Informed Extreme Learning Machines was successfully conducted by Scorsoglio et al. [2] for simulated data. In contrast to this Single Layer architecture our approach incorporates a Deep Feed Forward Neural Network topology with a physics informed loss function. As a real case scenario, wetest the machine learning algorithm on data of the Rosetta mission [3] orbiting comet 67P/Churyumov-Gerasimenko and present preliminary results of the study.AcknowledgementsThe project Artificial Intelligence for Precise Orbit Determination (AI4POD) is funded by Deutsches Zentrum für Luft- und Raumfahrt, Bonn-Oberkassel, under grant 50LZ2308.References[1] M. Raissi, P. Perdikaris, G.E. Karniadakis, Physics-informed neural networks: A deep learning framework for solving forward and inverse problems involving nonlinear partial differential equations,Journal of Computational Physics, Volume 378,2019, Pages 686-707, ISSN 0021-9991, https://doi.org/10.1016/j.jcp.2018.10.045[2] Scorsoglio, A., Ghilardi, L. & Furfaro, R. A Physic-Informed Neural Network Approach to Orbit Determination. J Astronaut Sci 70, 25 (2023). https://doi.org/10.1007/s40295-023-00392-w[3] Andert, T., Aigner, B., Dallinger, F., Haser, B., Pätzold, M., Hahn, M., 2024. Comparative Analysis of Data Preprocessing Methods for Precise Orbit Determination, in: EGU24-19558. Presented at the EGU General Assembly 2024, Vienna, Austria. https://doi.org/10.5194/egusphere-egu24-19558.
Modelling Lunar Impact Flashes from Molten Ejecta
Authors: Rice Paige , Luther Robert , Wünnemann Kai
Published: July 2024

Introduction: Lunar impact flashes have been observed from Earth since 1999 [1]. To date, over 600 impact flashes have been detected by individuals as well as multiple observation campaigns [2], including the NASA Lunar Impact Monitoring Program, the MIDAS project, and the NELIOTA project. The record of flashes has been analysed statistically to estimate the current near-Earth meteorite flux and size distribution [3], though the results of such estimates rely on some assumptions about the relationship between the radiative energy of the flashes and impactor velocity and kinetic energy.Luminous efficiency, the fraction of impactor kinetic energy that is transformed into light emission during the impact process, is a poorly constrained value. Common estimates range over three orders of magnitude, from 10-2 to 10-4 [4]. Recent modelling work produced a detailed model of the radiant process in the impact debris cloud and fit well to the observed flash using calculated impactor properties [5]. Their work builds on previous studies considering the physics of the radiant process, indicating that vaporized material in the instant of impact cannot provide enough thermal radiance to account for impact flash magnitude, and most of the light from impact flashes is created by thermal radiance of droplets of melted ejecta [1]. However, they did not fit their model to the observed diameter and depth of an associated crater. Method: We seek to improve the constraints on luminous efficiency by modelling simplified analogues of observed impact flashes with known associated craters. Here, we use the iSALE-Dellen shock physics code [6,7,8] to model the 17 March 2013 lunar impact flash and crater [Fig. 1], adjusting the impact parameters to best replicate the known factors of the impact and match the resultant crater size. Target porosity, modelled by the ε-α-porosity compaction model [8,9], is set at a homogeneous 42% and a vertical impact in a 2D cylindrical model is used for computational efficiency. We use the Drucker-Prager strength model and the ANEOS equation of state to model the lunar regolith. Then, we determine the volume of melted ejecta produced in each impact as a proxy for radiance, and vary velocity-mass balance and target porosity parameters to study the effect on ejected melt volume. Crater data permitting, we will also study additional, recently identified flash-crater pairs [10,11,12]. Figure 1: Crater identified with 17 March 2013 impact flash. a: before, b: after. [13]  Results: We show some preliminary results of our first study models in the plot below. Peak pressure on target material is plotted (in Pa x1e10). Material above the black curve is ejected as the model proceeds. All material is shown in position at t=0. The resolution of this model (10 CPPR) is not sufficient for a detailed analysis of peak pressure and melt volume; 40 CPPR resolution will yield a better result, reducing uncertainty to
The importance of gravity field spectrum for icy satellite interior structure determination: the case of Europa with the Europa Clipper mission
Authors: Cascioli Gael , Mazarico Erwan , Nimmo Francis , Dombard Andrew
Published: July 2024

A better understanding of the interior structure of icy moons in our Solar System is necessary to answer fundamental questions about their formation, evolution, and habitability. Until now, insights on the interior layering, core structure, and density distribution have been solely derived from global-scale gravity measurements, such as the mass, the moment of inertia (from the degree-2 static gravity field and/or obliquity), and the tidal gravity response. With the upcoming NASA Europa Clipper and ESA JUICE missions, we will obtain reliable estimates of the gravity field of Jupiter’s icy moons to higher degrees (shorter wavelengths).In this work, we present a new methodology and investigate the efficacy of utilizing the measured gravity field amplitude spectrum as an additional constraint in the inversion of the interior structure of differentiated icy bodies. After introducing and discussing the general methodology, we focus on Europa by considering the anticipated measurement accuracy of the Europa Clipper gravity and radio science investigation. We show that a Bayesian inversion of Europa’s interior that incorporates the measured gravity field spectrum offers much stronger determination of key geophysical parameters related to the interior structure of the body. In particular, it allows reliable constraints on the hydrosphere (ice shell and ocean) thickness, to within 10-20 km uncertainty, while at the same time reliably estimating key characteristics of the core, the silicate mantle, and the ocean floor, which is not possible with the traditional approach. The approach we present offers new sensitivity to the seafloor topography and elastic thickness, and it gives a way of probing the heat flow from the silicate interior. Ultimately, these fundamental constraints will help evaluate the potential for habitability of Europa and its subsurface ocean.Updating our previous work (Cascioli et al., 2024), we augment the inverse problem with the expected tidal constraints that Europa Clipper will derive, and we assess their beneficial role on the interior structure determination. Cascioli, G., et al. "Leveraging the Gravity Field Spectrum for Icy Satellite Interior Structure Determination: The Case of Europa with the Europa Clipper Mission." The Planetary Science Journal 5.2 (2024): 45.
Determining the sizes of selected asteroids with different techniques
Authors: Choukroun Antoine , Marciniak Anna , Ďurech Josef
Published: July 2024

Introduction:Determining the physical parameters of asteroids is a complex yet crucialtask in planetary science. Recent advancements in observational techniques andthe availability of vast data have led to the development of numerous analyticaland modelling approaches for parameter determination.In our research, we focused on studying several main-belt asteroids usinghigh-quality data. Initially, we modelled visible lightcurves using convex inver-sion (see [1] and [2]) obtaining precise information on the spin axis and an initialshape model. Subsequently, we used these results as input for another mod-elling technique called Convex Inversion Thermophysical Model (CITPM, see[3]). CITPM optimizes the model based both on lightcurves and thermal data,providing output such as surface roughness, temperature distribution, thermalinertia, and asteroid size. Additionally, by fitting the initial models to stellaroccultation observations, we determined asteroid sizes with another recognizedprecise method. This revealed a good agreement with the sizes determined byCITPM, enhancing the credibility of its other output parameters.Results:
As an example, we present here the results for one target: slowly rotatingasteroid (527) Euryanthe. The CITPM model for solution 1 and solution 2 areshown in Figure 1. Due to the mirror-pole ambiguity, we obtain two possiblesolutions (see [4]). Some of the parameters derived using the CITPM are givenin Table 1. Additionally, Figure 2 shows a fit of our models of (527) Euryantheto a stellar occultation by this asteroid observed on 2019-01-20. The best fit wasobtained for pole solution 2, and the corresponding size was found at 52.7 ± 1.8km.
Conclusions:The utilization of quality data has enabled the generation of reliable asteroidmodels. Furthermore, the supplementary use of the occultation observationtechnique, renowned for its accuracy in determining asteroid sizes, has provento be consistent with sizes determined via the CITPM technique. Without suchmodels as presented above, asteroid sizes tend to be determined with an orderof magnitude poorer accuracy.References: 
Speed and angular distribution of photodesorbed sodium at Moon and Mercury
Authors: Sarantos Menelaos , Tsavachidis Spiridon , Kuruppuaratchi Dona , Mierkiewicz Edwin
Published: July 2024

The release of sodium from regolith was simulated in order to elucidate the physical processes that generate surface-boundary exospheres in the inner solar system. Given the absence of laboratory experiments in relevant powders, a kinetic model used findings from experiments of Electron Stimulated Desorption (ESD) and Photon Stimulated Desorption (PSD) of adsorbates on single crystals to predict the angular distribution of photodesorption products from granular media. The regolith was simulated as a computer-generated sphere packing with grain size distributions selected from Luna and Apollo samples, while the effect of roughness at larger scales was also considered. The predicted angular distribution with this method varied as a function of solar inclination angle. Results were adopted into a global model of the sodium exosphere and compared to measurements from the Moon and Mercury.  Results indicate that small deviations of the speed distribution from a Maxwellian suffice to explain the lunar sodium measurements. However, measurements at Mercury appear to indicate a somewhat cooler speed distribution for PSD with a suppressed high-speed tail. We hypothesize that this difference in the sodium speed distribution from PSD between Mercury and the Moon could be attributed to the lower surface abundance of sodium adsorbates at the Moon.  
From Mars' Moons Formation to Submoons Hypothesis
Authors: Dahoumane Ryan , Lainey Valéry , Baillié Kévin
Published: July 2024

Our study focuses on the formation and evolution scenarios of the Solar system small satellites, utilizing a N-body simulation code based on the Gauss-Radau integrator (Everhart (1985)) with a particular emphasis on collision detection. We started benchmarking our code by comparing our simulations with the results of Hyodo et al. (2022). In a second step we extended their work by adding physical effects to evaluate the likelihood of Bagheri et al. (2021) Phobos and Deimos formation scenario. In a third step, we used it to evaluate the possibility for moons of the Solar system to host their own moon.Hyodo et al. (2022) argued that the formation of Mars’ moons based on a common progenitor fragmentation scenario as presented by Bagheri et al. (2021) was very unlikely. In fact, the former showed that under plausible assumption about the post-dislocation orbits of Phobos and Deimos based on the latter results, a collision between the two moons within 10 000 years is almost inevitable, leading to their annihilation. These outcomes were based on multiple N-body simulations considering Mars’ oblateness (J2 and J4 ) as well as mutual perturbations of point-masses moons.  We extended these findings by including new factors such as Sun gravitational perturbations, Mars’ axial precession and nutation, and its triaxial shape (sectoral terms). Additionally, we revised some of Hyodo et al. (2022) initial conditions regarding the distribution of Phobos and Deimos post-dislocation. Our results indicate that these additional influences do not significantly alter the outcome; Phobos and Deimos still converge towards collision on a similar timescale, reinforcing the improbability of their formation via progenitor dislocation.Furthermore, we have also used our integrator to assess the likelihood of subsatellite (moon of a moon) existence in the Solar system. By statistically analyzing collision and ejection probabilities of bodies orbiting some moons over extended periods, we identify potential candidates for discovering subsatellites. These findings provide valuable insights and targets for future observational efforts.
Figure 1: Cumulative fraction of collisions as a function of simulation time. The blue curve is a reproduction of Hyodo et al. (2022) result and the green curve represents the simulations with the additional effects mentioned above
 
 

References
  Amirhossein Bagheri et al. Dynamical evidence for phobos and deimos as remnants of a disrupted common progenitor. Nature Astronomy, 5(6):539–543, Jun 2021. ISSN 2397-3366. doi: 10.1038/s41550-021-01306-2.
 Edgar Everhart. An efficient integrator that uses gauss-radau spacings. International Astronomical Union Colloquium, 83:185–202, 1985. doi: 10.1017/S0252921100083913.
 Ryuki Hyodo et al. Challenges in forming phobos and deimos directly from a splitting of an ancestral single moon. The Planetary Science Journal, 3(8):204, 8 2022. doi: 10.3847/PSJ/ac88d2
 

 
 
 
Formation paths of binary asteroid systems born from YORP deformation
Authors: Dai Wen-Yue , Cheng Bin , Yu Yang , Baoyin Hexi , Li Jun-Feng
Published: July 2024

Many binary asteroid systems (‘Binary systems’) are believed to originate from Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) deformation; that is, the YORP spin-up of an asteroid triggers the rotational failure, and the material shed from the main body finally reaccumulates and forms its satellite(s). A binary system can form from a single YORP shedding event (‘SSh’), or from a sequence of such events (‘MultiSh’). In the latter one, a satellite formed in the first shedding event, thereby in the subsequent shedding events the evolution of shed material is influenced by the presence of this first-generation satellite. These different scenarios can result in various final configurations of binary systems. We aim to systematically investigate this relevance, and thereby obtain a ‘map’ of the various formation paths of binary systems.Our work primarily focuses on the MultiSh scenario, which is rarely concerned in previous works. We use 2 dimensionless parameters to characterize the perturbation effects of a satellite to the shed material. With semi-analytical investigation and discrete element method (DEM) simulations, we reconstructed the links between the character of an already-existed satellite and the final dynamical configuration of the binary system. Special attention is also paid to binary systems whose satellite itself is a contact-binary, such as the Dinkinesh system. We propose that this kind of binary systems can only form through some specific and interesting formation paths.This work has been supported by the National Natural Science Foundation of China grant No. 12372047.
An imprint of low-mass companions in the substructures of debris disks
Authors: Kim Minjae , Roccatagliata Veronica
Published: July 2024

Substellar companions and/or planets can have a significant impact on planetesimal and dust grain dynamics through gravitational perturbations, possibly causing several characteristic large-scale signatures such as gaps, misalignment, spiral density waves, and asymmetric radial/vertical density patterns in the density distribution of disk systems. Thus, tracing substellar companions such as planets or perturbers within debris disks can provide crucial insights and constraints into their evolution. While the direct detection of substellar companions in disk systems is challenging due to their small angular separation, the significant brightness contrast between a star and a planet, and the presence of small dust particles that dominate the continuum radiation across the entire spectral range, their existence can still be probed indirectly. Observable planet-disk configurations with large-scale signatures in the brightness distributions (e.g., spiral structures and/or two local azimuthal maxima) have been investigated using N-body simulations, smoothed particle hydrodynamics (SPH) simulations, and collisional evolution models of debris disk systems, both in the face-on and edge-on cases. In the present talk, we focus on the observable signatures that these interactions would leave on disks, using PHANTOM SPH code simulations. Furthermore, we will discuss the best observing strategies to detect the imprint in debris disk systems.