bluuebunny/crossref_metadata_2025 huggingface dataset:
La simplificación administrativa en México. Una necesidad cada vez mayor
Authors: López Fuentes Avelardo
Published: July 2024

La pretensión sobre este trabajo es exponer uno de los problemas que genera la burocracia en nuestro país, ya que si bien es cierto para la realización de un trámite existen normas aplicables, también lo es que la burocracia juega un papel importante en lo tardado y complicado que es realizar trámites administrativos. Existen tramites más complicados y tardados que otros, aunque uno podrá suponer que los tramites más sencillos son los menos tardados, pues bien, esto no es así. Ya que irónicamente por ejemplo el corregir una letra en el apellido o nombre de una persona nos lleva incluso en ocasiones a acudir a los tribunales civiles, es decir demandar al registro civil para que un juez le ordene al citado registro la corrección del acta. El desconocimiento de las leyes que exigen trámites, por ejemplo, para la apertura de un negocio es uno de los obstáculos más importantes, aunado al desconocimiento incluso de los servidores públicos encargados de realizarlo, lo cual provoca que transcurran muchos días para lograr la apertura de algún negocio. Con este trabajo se pretende exponer la necesidad de simplificar los trámites que deben efectuarse ante oficinas de gobierno, logrando con ello una tranquilidad en la población al obtener certeza jurídica, para ello es necesario estudiar la manera de lograr una autentica simplificación y con ello rapidez en los tramites que debemos realizar los ciudadanos.
Comunicación estratégica en la campaña electoral presidencial de Ecuador 2023: un estudio de la aplicación de las 22 leyes de Al Ries y Jack Trout en la estrategia política
Authors: Macías Ruiz María José , Cochea Panchana Gerson Alfredo
Published: July 2024

Este estudio se propuso examinar la implementación de las 22 leyes de Al Ries y Jack Trout en la estrategia de comunicación política durante la campaña presidencial de Ecuador en 2023. La metodología involucró una revisión exhaustiva de las redes sociales de los candidatos, centrándose en Facebook, Instagram y TikTok durante la segunda vuelta electoral. Los resultados destacaron que Luisa González empleó estrategias alineadas con las leyes de persuasión, exclusividad, liderazgo y escalera, mientras que Daniel Noboa Azín se destacó en consistencia, conexión y emoción. La conclusión principal reveló que la aplicación efectiva de estas leyes influyó significativamente en la construcción de la imagen de los candidatos, la percepción pública y la eficacia general de la comunicación estratégica en el proceso electoral. Esto subraya la importancia crucial de adaptarse a las dinámicas contemporáneas de la comunicación política, especialmente en el ámbito de las redes sociales, para lograr una conexión efectiva con el electorado y forjar una presencia sólida y diferenciada en la esfera pública.
The optical properties of stratospheric aerosol layer perturbation of the Hunga volcano eruption of January 15th, 2022
Authors: Sellitto Pasquale , Belhadji Redha , Legras Bernard , Podglajen Aurélien , Duchamp Clair
Published: July 2024

Abstract. The Hunga volcano violently erupted on January 15th, 2022, and produced the largest stratospheric aerosol layer perturbation of the last 30 years. One notable effect of the Hunga eruption was the significant modification of the size distribution (SD) of the stratospheric aerosol layer with respect to background conditions and other recent moderate stratospheric eruptions, with larger mean particles size and smaller SD spread for Hunga. Starting from satellite-based SD retrievals, and the assumption of pure sulphate aerosol layers, in this work we calculate the optical properties of both background and Hunga-perturbed stratospheric aerosol scenarios using a Mie code. We found that the intensive optical properties of the stratospheric aerosol layer (i.e., single scattering albedo, asymmetry parameter, aerosol extinction per unit mass and the broad-band average Ångström exponent) were not significantly perturbed by the Hunga eruption, with respect to background conditions. The calculated Ångström exponent was found consistent with multi-instrument satellite observations of the same parameter. Thus, the basic impact of the Hunga eruption on the optical properties of the stratospheric aerosol layer was an increase of the stratospheric aerosol extinction (or optical depth), without any modification of the shortwave and longwave relative absorption, angular scattering and broad-band spectral trend of the extinction, with respect to background. This highlights a marked difference of the Hunga perturbation of the stratospheric aerosol layer and those from other larger stratospheric eruptions, like Pinatubo 1991 and El Chichon 1982. With simplified radiative forcing estimations, we show that the Hunga eruption produced an aerosol layer likely 3–10 times more effective in producing a net cooling of the climate system with respect to Pinatubo and El Chichon eruptions, due to more effective shortwave scattering. As intensive optical properties are seldom directly measured, e.g. from satellite, our calculations can support the estimation of radiative effects for the Hunga eruption with climate or offline radiative models.
The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
Authors: Kiss Csaba , Müller Thomas , Marton Gábor , Szakáts Róbert , Pál András , Molnár László , Vilenius Esa , Rengel Miriam , Ortiz Jose-Luis , Fernandez-Valenzuela Estela
Published: July 2024

Recent stellar occultations have allowed accurate instantaneous size and apparent shape determinations of the large Kuiper belt object (50000) Quaoar and the detection of two rings with spatially variable optical depths. Here we present new visible range light curve data of Quaoar from the Kepler/K2 mission, and thermal light curves at 100 and 160 µm obtained with Herschel/PACS. The K2 data provide a single-peaked period of 8.88 h, very close to the previously determined 8.84 h, and it favours an asymmetric double-peaked light curve with a 17.76 h period. We clearly detected a thermal light curve with relative amplitudes of ~10% at 100 and at 160 µm. A detailed thermophysical modelling of the system shows that the measurements can be best fit with a triaxial ellipsoid shape, a volume-equivalent diameter of 1090 km, and axis ratios of a/b = 1.19 and b/c = 1.16. This shape matches the published occultation shape, as well as visual and thermal light curve data. The radiometric size uncertainty remains relatively large (±40 km) as the ring and satellite contributions to the system-integrated flux densities are unknown. In the less likely case of negligible ring or satellite contributions, Quaoar would have a size above 1100 km and a thermal inertia ≤ 10 J m−2K−1s−1/2. A large and dark Weywot in combination with a possible ring contribution would lead to a size below 1080 km in combination with a thermal inertia ≳10 J m−2K−1s−1/2, notably higher than that of smaller Kuiper belt objects with similar albedo and colours. We find that Quaoar's density is in the range 1.67-1.77 g cm−3, significantly lower than previous estimates. This density value closely matches the relationship observed between the size and density of the largest Kuiper belt objects. Figure 1: Thermophysical model results for Quaoar. Left: All available IR observations divided by the corresponding TPM predictions, using a triaxial shape with an equivalent diameter of 1090 km, and a thermal inertia of 12 J m−2K−1s−1/2 . The calculations take small flux contributions from the ring and Weywot into account. These absolute ratios are very sensitive to the size and thermal inertia assumptions in the model, the 24 μm points is strongly influenced by surface roughness effects. Right: Far-infrared light curves. The small ring and Weywot flux contributions are subtracted from the observed PACS 100 and 160 μm lightcurve data. The triaxial Quaoar model solutions (at 100 μm in green and at 160 μm in orange) are shown on top. The boxes represent the mean PACS values.
Mars Express and ExoMars Trace Gas Orbtiter - mission status & science highlights
Authors: Wilson Colin
Published: July 2024

Mars ExpressMore than two decades after its launch in June 2003, Mars Express remains a dependable, highly productive and innovative mission.Recent science highlights include (1) continued mapping of subsurface reflectors beneath the south polar layered ice deposits, and associated work to explain the cause of these reflections; (2) a global map of minerals on Mars with 200 m/px resolution, obtained from analysis of infrared spectra; (3) release of 50 m resolution Digital Elevation Models based on HRSC stereo topography for quadrangles covering an ever-increasing proportion of the global surface; (4) a global climatology of ozone and water from both nadir and occultation observations and its relation to atmospheric dust; (5) transient atmospheric phenomena, such as a recurrent orographic cloud feature at Arsia Mons; (6) detailed investigation of the ionospheric structure, its variability, and coupling to the lower atmosphere; (7) continued monitoring of both the upstream solar wind conditions and of downstream escaping ions; (8) detailed study of Phobos during flybys at altitudes as low as 50 km.Spacecraft and instrument teams continue to implement new and improved observation modes. One example is new MARSIS instrument software which now allows raw data to be returned from much longer subsurface sounding passes, improving the search for basal reflectors beneath polar ice caps; another example is mutual radio occultation observations between Mars Express and ExoMars Trace Gas Orbiter, potentially providing vertical profiles of ionospheric electron content with good spatial and temporal coverage.ExoMars Trace Gas OrbiterTGO has now completed almost three full Mars years since reaching its science orbit in April 2018.Highlights include (1) continuing non-detection of methane, with upper limits as low as 20 ppt by volume. Reconciling this continued non-detection by TGO with the background levels of several hundred ppt in Gale crater by MSL remains an enigma, stimulating further research. (2) detection of HCl, the first reported halogen-containing species in the atmosphere of Mars. (3) further detail of the transport of water to high altitudes, a critical step in the escape of water from Mars. and (4) continued acquisition of 5 m colour imagery and digital elevation models over a wide range of terrain and target types, including landing site characterization.Funding for extending both missions was recently secured and is currently in place until end 2026 (Mars Express) and end 2025 (Trace Gas Orbiter).
Super-Earth formation in compact disks around M dwarfs
Authors: Sanchez Mariana , van der Marel Nienke , Lambrechts Michiel , Mulders Gijs , Guerra-Alvarado Osmar
Published: July 2024

M dwarfs are the most common stars in our solar neighborhood. Due to the improvements in radial velocity and transit techniques, we know that rocky planets, in particular close-in super-Earths, in compact configurations are the most common ones around M dwarfs. On the other hand, thanks to the high angular resolution of ALMA we know that most disks around very low mass stars are rather compact and small, which favors the idea of an efficient radial drift that could enhance planet formation in the terrestrial zone. Motivated by these results, we have investigated rocky planet formation around M dwarfs driven by pebble accretion through N-body simulations. We assumed that planet formation took place in compact dust disks caused by efficient dust radial drift. In the simulations we incorporated planet-disk interactions and tidal and relativistic corrections that include the evolution of the luminosity, radius and rotational period of the star. For our standard model we used different gas-disk viscosities and initial embryo distributions. For different stellar masses we also studied planet formation by planetesimal accretion. Our main result is that the sample of simulated planets that grow by pebble accretion in a gas-disk with low viscosity can reproduce the low-mass exoplanet population around M dwarfs in terms of multiplicity, masses and semi-major axis. Furthermore, we found that a gas disk with high viscosity can not reproduce the observed planet masses. Also, we show that planetesimal accretion favors the formation of water worlds and small planets that so far have not been detected. This work points towards a new approach for the disk conditions needed to study rocky planet formation around M dwarfs.
Exploring the sulfate-bearing unit: Recent ChemCam results at Gale crater, Mars
Authors: Gasnault Olivier , Schroeder Susanne , Cousin Agnes , Frydenvang Jens , Hughes Emmy , Dehouck Erwin , Rammelkamp Kristin , Johnson Jeffrey , Rapin William , Lanza Nina , Wiens Roger C. , Maurice Sylvestre ,   ChemCam science team
Published: July 2024

The Curiosity rover of the Mars Science Laboratory mission is exploring Gale crater on Mars since August 2012 [Vasavada2022]. On board, the ChemCam instrument [Wiens2012, Maurice2012] combines Laser-Induced Breakdown Spectroscopy (LIBS), passive spectroscopy and imaging.ChemCam is a remote sensing instrument, assessing the chemical composition of rocks and soils up to a few meters from the rover, imaging outcrops at longer distances, and surveying the atmospheric variability. The chemistry of primary and secondary phases is obtained using LIBS by performing typically five point rasters on the martian targets. Each point is investigated with 30 laser shots. This technique can therefore highlight some elemental correlations [Rammelkamp2024], or even some depth variations (
Asteroid Classification with GAIA: Machine Learning Insights from Reflectance Spectra
Authors: Anghel Simon , Merin Bruno , Kueppers Michael
Published: July 2024

Asteroids are diverse objects found in the Solar System, populating in large numbers the near-Earth space, yet most of them form the main belt. While upcoming observatories promise frequent observations of asteroids to compute their orbit, understanding their physical composition remains a challenge due to the inherent difficulty in obtaining spectra.Launched in 2013, GAIA satellite repeatedly scans the entire sky, not only mapping the more than 1 billion stars, but also discover and measure exoplanets, asteroids, comets and planetary satellites in our Solar System. For the asteroids and comets, GAIA provides more accurate astrometry, photometry as well as albedo and spectra.In this study we accessed the freely available GAIA Solar System Objects reflectance spectra in the visible range (418-990 nm) and built a catalogue of their spectral wavelengths. After thresholding for the well calibrated spectras we tested 8 unsupervised machine learning (ML) models to cluster the spectras into classes.After fine hyperparameter tuning of the models we found that several ML methods capture well the features of the already classified asteroids. Also, we obtained a spectral classification for the unclassified asteroids observed by GAIA.The next step is to extend the study by employing the dynamical features and the albedo to better constrain the asteroid families, and ultimately, to understand distribution of the asteroids in the Solar System.Acknowledgements: SA was supported during this work by the ESA Archival Research Visitor Programme.
Investigating chemical and mineralogical biosignatures in microbialites from Laguna Negra, Argentina
Authors: Maldanis Lara , Areias Camila , J. Gomez Fernando , Thoury Mathieu , Sánchez-Róman Mónica
Published: July 2024

The Laguna Negra, a high-altitude hypersaline close-basin lake in the Andes of Northwest Argentina, presents a unique environment for studying the formation of microbialites (Gomez et al., 2014; Buongiorno et al., 2019). The extreme conditions like high UV radiation and salinity restrict multicellular life, allowing microbial activity as one of the drivers of carbonate precipitation. Oncolites samples, interpreted as a result from fluid mizing and biologically mediated nucleation (Buongiorno et al., 2019) and collected under Europlanet project have been analyzed for the search of chemical and mineralogical biosignatures. Synchrotron µ-X-Ray Fluorescence provided major-to-trace elemental distributions, revealing elements concentrated in stromatolitic laminae (e.g., Sr, Co, Rb, Mo, Pb), concentrated in not strictly stromatolitic laminations (eg., Fe, Mn, Mo, Ni, As, Pb, Zn), and contrasting with the elements widespread in the matrix (e.g., Ca, Cl, Br, K T, V). UV photoluminescence macroscopy highlighted laminations invisible in naked eye, providing also complementary information of chemical differences. Synchrotron scanning SAXS/WAXS maps provided additional information on mineral composition and crystallites shape and orientation. These combined results provide complementary chemical and mineralogical information for the characterization of the biotic and abiotic layers involved on the oncolites accretion, allowing us to define combination of characters specific to microbially-mediated precipitations. This work also opens the way for the multiscale assessment of mineral biosignatures of microbial precipitation in laminated rocks, from Earth or elsewhere.Figure 1. a) UV photoluminescence macroscopy of the Laguna Negra cross-cut oncolite excited at 385 nm. Emission collected at 571 nm (red), 708 nm (green) and 835 nm (blue). B) Synchrotron XRF map of Sr (red), Zn (green) and Ca (blue). Stromatolitic layers are rich in Sr, while Zn is restricted to outer, likely evaporitic layers. References:Buongiorno, J. et al. (2019) ‘Mineralized microbialites as archives of environmental evolution, Laguna Negra, Catamarca Province, Argentina’, Geobiology, 17(2), pp. 199–222. Available at: https://doi.org/10.1111/gbi.12327.Gomez, F.J. et al. (2014) ‘Microbialites in a high-altitude Andean lake: Multiple controls on carbonate precipitation and lamina accretion’, Palaios, 29(6), pp. 233–249. Available at: https://doi.org/10.2110/palo.2013.049.
Unraveling Double-Layered Ejecta: Lessons from Lonar Crater and Beyond
Authors: Wilk Jakob , Agarwal Amar , Dey Gourab
Published: July 2024

Comparative planetological studies suggest that subsurface fluidization during ejecta emplacement may play a significant role in the formation of double-layered ejecta (DLE) craters, not only on Mars but potentially on other planetary bodies like Ceres or Ganymede. On Mars, DLE crater formation likely involved water or water-ice in the near-surface substrate. For the formation process it is hypothesized that volatile-rich rock debris flows driving the outer layer's emplacement and the inner layer moving as a translational slide.This process results in two superimposed ejecta morphologies with striated surfaces, rampart, and moat structures. Although morphological features, especially the ejecta blankets, have largely been destroyed for most terrestrial impact structures, recent studies have revealed that Lonar crater in India, Ries crater in Germany, and Bosumtwi crater in Ghana possess ejecta ramparts similar to Martian DLE impact craters.In this study we can show the typical striated DLE morphologies to be preserved in the subsurface contact of the different ejecta layers for the Ries crater and suggest that this might be the case for other terrestrial DLE craters as well, as long as multiple layers can be found. In a recent field study, we were able to confirm the presence of two distinct ejecta layers at least for Lonar crater in India, similar to the Ries crater in Germany. Additionally, we conducted a detailed study involving drone photogrammetry, rock magnetics, micro-fracture network analysis, and geophysical investigations using a 100 MHz bi-static ground-penetrating radar (GPR) system at Lonar. These findings were compared to similar observations made for the ejecta of the Ries crater in Germany, where additional electric resistivity tomography (ERT) corroborates the findings of the GPR.By studying terrestrial analogs, such as Lonar crater, we aim to constrain boundary conditions for DLE crater formation on other planets, specifically regarding the volatile content of the affected crust. Lonar, with its smaller diameter compared to Martian DLE craters, offers valuable insights into DLE formation variability. Moreover, Lonar can serve as an analogue laboratory for Martian DLE craters in basalt regions such as Hesperia Planum. Lastly, our findings shed light on the temporal variability of landforms in connection to the formation conditions required for DLE craters on Mars, which mostly occur at mid-latitudes and scarcely in the southern hemisphere, mirroring past climatic evolution for both Ries and Lonar crater. 
Time-Domain Spectroscopy: an emerging alternative to Raman and FTIR Spectroscopy in Space Exploration?
Authors: Gensch Michael , Ha YooKyung , Woeste Jonas , Azih Dominic , Pavlov Sergey , Stojanovic Nikola
Published: July 2024

Robotic missions to extraterrestrial objects in our solar system are nowadays often equipped with instruments allowing to explore the geochemistry of the surfaces by e.g. identification of their characteristic vibrational fingerprints. Femtosecond lasers have in recent years been shown to be in principle space qualified, opening up the opportunity to explore the potential of different time-domain techniques as compact, robust alternatives to e.g. Raman spectroscopy or FTIR spectroscopy [1,2]. In this contribution the potential of two time-domain techniques: (i) coherent phonon spectroscopy (CPS) and (ii) THz Time-Domain Spectroscopy (THz-TDS), as emerging in-situ spectroscopic techniques to identify solids by their characteristic  phonon spectra is discussed based on exemplarily measurements of different (planetary) materials. It is shown that: (i) CPS can give access to the raman-active phonon spectra equibvalent to Raman spectroscopy but is not hampered by fluorescence backgrounds and (ii) THz-TDS allows to probe the infrared-active fingerprint of matter while avoiding bulky (cryogenic) spectrally broadband infrared detectors. It is outlined how the bandwidth of the techniques is related to the available laser pulse duration. CPS and THz-TDS measurements with a bandwidth of beyond 1000 cm-1 (30 THz) and a resolution of better than 4 cm-1 (100 GHz) are demonstrated and compared to complementary Raman and FTIR measurements.[1] J. Lee et al, Testing of a femtosecond pulse laser in outer space. Scientific Reports (2014); 4, 5134.[2] M. Lezius et al, Space-borne frequency comb metrology. Optica (2016); 3, 1381.[3] O. Gueckstock et al, Radiation hardness of ultrabroadband spintronic terahertz emitters: en-route to a space-qualified terahertz time-domain gas spectrometer, Applied Physics Letters (2024); 124, 141103.
Thermal Infrared Imager (TIRI) Simulation with Kalast for Hera Flyby Targets
Authors: Henry Grégoire , Karatekin Özgür , Senel Cem Berk
Published: July 2024

Information about the formation of the Solar System and the history and geological processes of the Earth can be found studying the nature of asteroids. Understanding asteroids properties and mechanical behavior is required for planetary defense. Asteroid thermophysical properties such as thermal inertia, grain size, porosity, and surface material can be effectively constrained through thermophysical modelling combined with observations. Infrared data contributes significantly to determining reliable asteroid shapes and spin states.Recent observations of thermal infrared imager (TIR) onboard the Hayabusa 2 spacecraft revealed the highly porous nature of the C-type asteroid Ryugu. OSIRIS-Rex infrared instruments OTES and OVIRS provided valuable information about Bennu asteroid. Both missions realized touchdown on the asteroids to collect samples and the resulting mechanical behavior from the contact could not be expected. Looking forward, the HERA mission is the next small body mission equipped with a thermal imager TIRI based on TIR with better characteristics flying towards the binary asteroid system (65803) Didymos. TIRI will be used to take images and infrared measurements of the binary asteroid Didymos. HERA is launched with two cubesats with the intention to characterize Dimorphos the moon of the binary system from a closer distance and will attempt a landing.HERA will be launched in October 2024 and swing-by Mars in March 2025. The mission will provide a unique opportunity for calibration of the TIRI instrument and measurement of the bodies.Here we present the simulation of those observations with Kalast, the new thermophysical model designed specifically for binary asteroids at the Royal Observatory Belgium. The tool enables in-depth analysis of thermophysical characteristics for asteroids. The model is generic for small bodies and capable of simulating binary systems, incorporating factors, such as mutual and self-heating. By utilizing shape models to accurately represent surface features, the model computes shadows for accurate illuminations. Moreover, the model simulates the thermal flux of the asteroids, considering occultation from an observer viewpoint. Roughness is being implemented to correct observed infrared flux. Whether observed through a spacecraft camera or a ground-based telescope, Kalast is capable of simulating light curves in visible and in infrared. More generally, Kalast can simulate images taken by spacecraft also in visible and infrared. Kalast is designed for the inversion of infrared measurements data obtained from thermal instruments onboard missions targeting asteroids.
Europa-UVS at One Month Prior to Europa Clipper Launch
Authors: Retherford Kurt , Becker Tracy , Greathouse Thomas , Gladstone Randy , Freeman Matthew , Davis Michael , Giles Rohini , Kammer Joshua , McGrath Melissa , Brooks Shawn , Raut Ujjwal , Mamo Bereket , Hendrix Amanda , Hue Vincent , Ferrell Sue , Johnson Erica , Molyneux Philippa , Persson Kristian , Roth Lorenz , Saur Joachim ,   Europa-UVS Team
Published: July 2024

The Europa Clipper mission will launch in October 2024. The Europa Ultraviolet Spectrograph (Europa-UVS) instrument science goals are focused on Europa habitability goals, specifically: 1) Search for and characterize the vapor composition of any plumes; and 2) Enable mapping of atmospheric vertical structure and composition. We’ll discuss the status of the Europa-UVS instrument, plans for post-launch commissioning and calibrations, and its extreme-UV to far-UV (55-205 nm) observational techniques to investigate aurora and airglow imaging, stellar and solar occultation, Jupiter transit, and surface reflectance.  Coordination with its sister instrument on the Juice mission, JUICE-UVS, offers additional opportunities for advancing the science goals for each mission.
Solar System Minor Bodies in theJavalambre Variability Survey DR1: The catalog
Authors: Morate David , Mahlke Max , Álvarez-Candal Álvaro , Ederoclite Alessandro , Vázquez Ramió Héctor
Published: July 2024

The Javalambre VARiability Survey (J-VAR) is a photometric survey that is being carried out with the 0.8m Javalambre Auxiliary Survey Telescope (JAST80), located at the Observatorio Astronómico de Javalambre (OAJ, in Teruel). J-VAR is the time-domain extension of the Javalambre-Photometric Local Universe Survey, J-PLUS, carried out in the same telescope. J-VAR uses a sub-set of seven filters from the J-PLUS set covering the range from 0.395 up to 0.861 microns, including the g,r,i filters from the SDSS set. The main concept of J-VAR is to explore the time-domain capabilities offered by the JAST80, and its strategy is as follows: each field is observed three times, with dithering, in all seven filters, and is revisited a total of ten times whenever the weather conditions allow J-VAR to be executed. This observational strategy, favouring the detection of transient phenomena, is also well-suited for the detection of small bodies (SBs) of the Solar System.Within the 101 fields included in J-VAR Data Release 1 we have recovered more than 130,000 individual detections (an asteroid was detected in one image). These correspond to more than 8,600 objects (a total of 6,572 individual asteroids). The detection of the SBs is done using the SOSS pipeline (Mahlke et al. 2019). Here, we present the first catalog of small bodies of the Solar System observed with J-VAR: we show the calibration method, we present some statistics on the data, and we outline the next steps for future iterations of the catalog.
Preliminary Results of the Categorizing and Statistical Survey of Martian Ionospheric Irregularities
Authors: Wan Xin , Zhong Jiahao , Xiong Chao , Cui Jun
Published: July 2024

A climatological survey of Martian ionospheric plasma density irregularities was conducted by exploring the in-situ measurements of the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. The irregularities were first classified as enhancement, depletion, and oscillation. By checking the simultaneous magnetic field fluctuation, the irregularities have been classified into two types: with or without magnetic signatures. The classified irregularities exhibit diverse global occurrence patterns, as those with magnetic signatures tend to appear near the periphery of the crustal magnetic anomaly (MA), and those without magnetic signatures prefer to appear either inside of the MA or outside of the MA, depending on the type and solar zenith angle. Under most circumstances, the irregularities have a considerable occurrence rate at altitudes above the ionospheric dynamo height (above 200 km), and the magnetization state of the ions seems irrelevant to their occurrence. In addition, the irregularities do not show dependence on magnetic field geometry, except that the enhancement without magnetic signatures favors the vertical field line, implying its equivalence to the localized bulge (Duru et al., 2006). Other similarities and discrepancies exist in reference to previous studies. We believe this global survey complements previous research and provides crucial research clues for future efforts to clarify the nature of the Martian ionospheric irregularities.
Ground-based Optical Interferometry to Characterize Exoplanets
Authors: Lacour Sylvestre , Le Bouquin Jean-Baptiste
Published: July 2024

Dual-field interferometry, enabled by the GRAVITY instrument at the Very Large Telescope Interferometer, achieves very high contrast at very small separations. It has directly detected exoplanets, such as Beta Pictoris b, which are beyond the reach of other instruments. This presentation will provide a brief history of the technique, discuss recent advancements leveraging Gaia astrometry, and explore future prospects in light of upcoming Gaia data releases, the Extremely Large Telescope (ELT), and future space missions.
Internal structure of Water-rich planets
Authors: Lozovsky Michael , Vazan Allona
Published: July 2024

Water is expected to be abundant component in planetary interiors, particularly in sub-Neptune planets, whose radii suggest the presence of volatiles in their atmospheres. However, directly observing the precise water mass fraction and water distribution remains unfeasible. In our study, we employ an internal structure code to model planets with high water content and explore potential interior distributions. Departing from traditional assumptions of a layered structure, we determine water and rock distribution based on water-rock miscibility criteria. We model wet sub-Neptunes with an iron core and a homogeneous mixture of rock and water above it. At the outer regions of the planet, the pressure and temperature decrease below the rock-water miscibility point (the second critical point), causing the segregation of water and rock. Consequently, a shell of water is formed in the outermost layers, resulting in a subsequent manifestation as a gaseous water atmosphere. By considering the water-rock miscibility and the gaseous state of water, our approach holds significant implications for estimating the water mass fraction of detected exoplanets.We model two extreme cases: a fully homogeneous mass-rock envelope surrounding an iron core, and a more traditional three-layer structure where water and rock are separated. In both cases, the outermost water layers form an atmosphere.  With various equilibrium temperatures and masses, assuming different structures, we calculate different radii for various scenarios. Planetary interiors are modeled using a modified version of the Magrahtea code (Huang et al., 2022). With these tools, we model the internal structure of a sample of exoplanets (L 98-59 d, TOI-1685 b, TOI-776 b, TOI-270 d, K2-146 b, K2-146 c).
On the Outer Solar System moon-magnetosphere interactions: the unique case of Ganymede
Authors: Plainaki Christina
Published: July 2024

Thanks to the analysis of data obtained during past and current missions to the outer solar system, as well as telescope observations of giant planets and their moons, our knowledge on the moon-magnetosphere interactions has been singificantly grown in the recent years. Theoretical progress in the field of space plasma physics and the performance of numerical simulations have significantly contributed in our better understanding of the near-moon environments and the underlying physical processes as well as their variability both at long and short terms. There is a wide variety of moon environments in the outer solar system depending both on the bodies properties and the specific characteristics of the planetary magnetosphere in which they are embedded. Although each case of moon-magnetosphere interaction is unique, a comparative planetary science context can often result useful in our overall understanding of the related physical processes. The interaction between Ganymede and its surrounding plasma environment is of special interest, mainly because this moon possesses its own mini-magnetosphere. Reconnection allows Jovian plasma and energetic ions to access the moon’s surface where they precipitate following patterns that depend on the position of Ganymede with respect to the Jupiter plasma sheet. An in depth understanding of the properties of the plasma-magnetosphere interactions in the vicinity of Ganymede will reveal the details determining the ion-surface processes responsible for the exosphere generation as well as the weathering and the surface evolution history.In this review, some paradigms of moon-magnetosphere interactions in the outer solar system will be discussed and special emphasis to the unique case of Ganymede will be given. The role of comparative science in getting the global picture and addressing long-lasting open questions in this field will be also addressed.
Oxides and Reduced Phases in the Mid-IR: Data for the BepiColombo Mission to Mercury 
Authors: Morlok Andreas , Weber Iris , Reitze Maximilian P. , Stojic Aleksandra N. , Klemme Stephan , Pasckert Jan H. , Bauch Karin E. , Hiesinger Harald , Helbert Jörn
Published: July 2024

Introduction: The MERTIS (MErcury Radiometer and Thermal Infrared Spectrometer) onboard of the BepiColombo ESA/JAXA mission to Mercury is a mid-infrared instrument that will allow mapping the hermean surface from 7 µm to 14 µm [1,2]. After arrival in 2025, a database for the interpretation of the data is needed. As part of this effort, we have studied rock samples like impact rocks and meteorites [e.g,. 3]. A second field of interest are analogs synthesized based on data by MESSENGER [e.g., 4].Based on recent modeling of the oxidation state of the hermean surface, a highly reducing environment can be expected [5,6]. Likewise past volcanism or impact experiments suggest the presence of extremely reduced phases, e.g., Si-metal (e.g, 7, 8]). This implies that in addition to common minerals (pyroxene, plagioclase), also oxides (corundum, spinel, periclase), metallic phases, halides, and reduced variations e.g. of olivine (Ca-olivine Larnite) are possible. As part of our database project, we cover this type mineral phases.Samples and Techniques: We characterized the materials first with EMPA. Samples were ground and sieved into grain four size fractions (
Investigating the Formation of Complex Organic Molecules in the Protosolar Nebula and Their Incorporation into the Galilean Moons
Authors: Benest Couzinou Tom , Amsler Moulanier Alizée , Mousis Olivier
Published: July 2024

The outer solar system bodies, including the Galilean moons, are expected to have accreted carbonaceous material during their formation. This carbonaceous material is likely composed of Complex Organic Molecules (COMs), whose formation could have taken place in the protosolar nebula. During their journey through the disk, icy pebbles may have been exposed to different interstellar UV irradiation and temperature conditions, which could have led to the formation of COMs, as experimental studies under similar conditions have demonstrated.Regarding the formation of the Galilean moons, several scenarios are possible. This study focuses on the formation of the moons in a cold circumplanetary disk, implying that the building blocks originating from the protosolar nebula are not altered by the circumplanetary disk, and their composition is determined solely by the thermodynamic conditions of the protosolar nebula.The aim of this study is to investigate whether the thermodynamic conditions in the disk were consistent with the formation of COMs in the environment where the Galilean moons formed. To achieve this, the following approach has been taken:  two-dimensional model has been developed to compute the transport of particles within the protosolar nebula using a Lagrangian scheme. This model deduces the accumulated irradiation dose along the particles' paths.
based on experimental data, the model demonstrates that a small fraction of particles consistently transports COMs within the Jupiter region.
By combining theoretical modeling and experimental data, this study aims to shed light on the potential formation and incorporation of COMs into the Galilean moons during the early stages of the solar system's evolution.
Direct Detection of Ongoing Magnetic Reconnection at Mercury's High-Latitude Magnetopause
Authors: Wang rongsheng , CHeng Zihang , Slavin James A. , Lu Quanming , Raines Jim , Lu San , Guo Jin , Gonzalez Walter
Published: July 2024

An ongoing magnetic reconnection event was detected in the Mercury's high latitude magnetopause during a northward interplanetary magnetic field. The reconnection X-line region was revealed in the Mercury's magnetopause based on the encountered flux ropes ejected away from this region both planetward and tailward. A series of magnetic flux ropes, known as flux transfer event shower were observed tailward of this X-line region. These flux ropes were probably expanding and deflected as they were ejected away tailward from the X-line region. Large-amplitude variations in all three components of the magnetic field and a few small-scale flux ropes were observed inside the X-line region, which could be the seed of the flux rope shower at the magnetopause. The observations suggest that magnetic reconnection is highly dynamic and persistent in Mercury's magnetosphere.
Generic Entry Probe Program (GEPP) – an international initiative promoting the development of European descent modules dedicated to the in situ exploration of giant planets
Authors: Mousis Olivier ,   GEPP team
Published: July 2024

The international consortium GEPP has been set to conceptualize probe designs with appropriate payloads that would remain within the typical budget allocated for ESA M-class missions (currently 500 M€). The aims of the consortium are i) to conceptualize a line of generic planetary entry probes, ii) to make the international science community, ESA and its member states, conscious that there is an opportunity to supply a series of entry probes as part of future international collaborations, and iii) to demonstrate that an M-class budget could possibly fund several entry probes with well-prioritized science objectives. A line of conceptualized generic planetary entry probes could be targeted to the giant planets with very few modifications, and collaborations could include the future NASA flagship mission towards Uranus (Uranus Orbiter Probe) or to any future NASA-led mission to the outer planets for an affordable budget. The model payload capabilities of each concept will be defined according to a carefullydesigned science traceability matrix. Two extreme concepts shall be investigated by the GEPP Consortium, namely a highly capable parachute-descent probe including a typical payload of 30 kg of scientific instruments down to 10 bars, and a smaller parachute-descent probe designed to address top priority science objectives with selected key measurements that would address the ESA Voyage 2050 science objectives. This presentation will detail the scientific objectives for each entry probe concept design, as well as the content, organization and planning of the study, which is assumed to be completed by the end of 2025.
 
The Advanced Small Analyzer for Neutrals (ASAN) instrument on Chang’E-4: A review of five years on the lunar surface
Authors: Wieser Martin , Barabash Stas , Wang Xiao-Dong , Williamson Hayley , Stenberg-Wieser Gabriella
Published: July 2024

The Advanced Small Analyzer for Neutrals (ASAN) instrument [1] is the first instrument to measure energetic neutral atoms directly on the lunar surface. Installed onboard of the Yutu-2 rover of the Chinese Chang’E-4, mission it started operations in January 2019. The landing site in the Karman crater on lunar far side is at the edge of the large magnetic anomaly in the South Pole-Aitken basin. The ASAN instrument has been operated periodically since, making use of the mobility of the rover to get different observation geometries.When the solar wind interacts with the lunar surface, a portion of it is reflected back as energetic netural atoms. Previous studies have provided evidence of neutral hydrogen atoms [2] and solar wind protons being reflected from the surface. However, prior to ASAN, all these measurements were performed form orbit and no direct measurements on the surface had been conducted. ASAN’s observation location directly at the surface allows to investigate the microphysics of the solar wind-surface interaction process and to study the effects of local magnetic anomalies on the emitted energetic neutral particle flux.The ASAN instrument is an 8th generation instrument of the SWIM family [3]. ASAN uses a charge conversion surface to convert energetic neutral atoms to positive ions and analyzed them with s surface-interaction based time-of-flight system combined with an electrostatic analyzer and an electrostatic elevation scanning system. This enables ASAN to to measure the direction-, energy-, and mass-resolved energetic neutral atom flux on the surface.We report on the instrument status and present a review of energetic neutral atoms observations done by ASAN on the lunar surface and discuss possible implications for the near-surface plasma environment. [1] M. Wieser, S. Barabash, X.-D. Wang, A. Grigoriev, A. Zhang, C. Wang, and W. Wang. The Advanced Small Analyzer for Neutrals (ASAN) on the Chang’E-4 Rover Yutu-2. Space Science Reviews, 216(4):73, 2020.[2] 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.[3] M. Wieser and S. Barabash. A family for miniature, easily reconfigurable particle sensors for space plasma measurements. Journal of Geophysical Research: Space Physics, 2016 
JWST observations constraining the population of planets in debris disc systems with gaps
Authors: Bendahan-West Raphael
Published: July 2024

Combining the resolved observations of debris discs with ALMA and the enhanced sensitivity of JWST presents a unique opportunity to deepen our understanding of planetary systems. Over the past 5 years, ALMA has revealed substructures within debris discs, suggestive of planetary influence, yet the direct detection of these putative planets remains elusive. Now with JWST's advanced capabilities, we have an unprecedented opportunity to detect the population of planets at 10s of au currently inferred by ALMA.While only three debris discs have shown gaps so far, we are becoming more aware that these gaps might be common. Similar to observations in our Solar System, the presence of gaps in debris components hints towards the presence of planets. These gaps could either be carved by planets in situ or by inner planets exercising secular resonances.In this talk, I will present JWST Cycle 1 MIRI 11um observations targeting three known debris discs with gaps: HD107146, HD92945, HD206893. I will show how planet-disc interactions combined with astrometric accelerations allow us to constrain the population of planets in the inner regions of these systems, at the disc inner edge and in the gap location, ultimately evaluating the degenerate scenarios proposed as the origin of these gaps.
Classification of Martian pyroxenes with wide-coverage CRISM multispectral datasets
Authors: Roivainen Matti , Aranha Malcolm
Published: July 2024

A renewed interest in human presence in extraterrestrial regions is evident from the number of crewed missions planned in the near future. A continued presence will require locally sourced raw materials, making exploration critical. Pyroxene composition is a key factor in the evolution of magmatism on the Martian surface and a crucial indicator of mineralization related to ultramafic-mafic deposits. This study develops a remote classification method for pyroxenes based on the equations proposed by Gaffey et al. (2002), utilizing the connection between the centers of absorption features and the molar concentrations of ferrosilite (Fs) and wollastonite (Wo). A 72-channel multispectral surveying mode and a 489-channel targeted hyperspectral mode of the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) are used in four vast study areas spanning the southern highlands to demonstrate the capability of multispectral data-based classification on a global scale. The results indicate dominance of Mg-rich augite and pigeonite in the study areas while demonstrating the method's sensitivity to different types of terrains. The technique can effectively identify regions of Mg-rich surfaces. It can be applied to hyperspectral data and is not sensor-specific, making it widely applicable on Mars and all planetary bodies with available spectral data. The classification results from this technique can aid future mineral exploration on all applicable targets.
Is Saturn a failed gas giant?
Authors: Helled Ravit
Published: July 2024

The formation history of giant planets inside and outside the Solar System remains unknown. We suggest that runaway gas accretion is initiated only at a mass of ∼100 M⊕ and that this mass corresponds to the transition to a gas giant, a planet whose composition is dominated by hydrogen and helium. Delayed runaway accretion (by a few million years) and having it occurring at higher masses is likely a result of an intermediate stage of efficient heavy-element accretion (at a rate of ∼10−5 M⊕ yr−1) that provides sufficient energy to hinder rapid gas accretion. This may imply that Saturn has never reached the stage of runaway gas accretion and that it is a “failed giant planet”. The transition to a gas giant planet above Saturn’s mass naturally explains the differences between the bulk metallicities and internal structures of Jupiter and Saturn. The mass at which a planet transitions to a gas giant planet strongly depends on the exact formation history and birth environment of the planet, which are still not well constrained for our Solar System. In terms of giant exoplanets, the occurrence of runaway gas accretion at planetary masses greater than Saturn’s can explain the transitions in the mass-radius relations of observed exoplanets and the high metallicity of intermediate-mass exoplanets.