bluuebunny/crossref_metadata_2025 huggingface dataset:
The relationship between the level of resilience and coping strategies among disabled convicts
Authors:   University of the FPS of Russia, DYACHKOVA YULIA E.
Published: July 2021

The article presents a study of the phenomenon of the resilience of convicts with disabilities. The purpose of the research is to study the features of the manifestation of resilience and coping strategies among disabled convicts in correctional institutions of the FPS of Russia Main Department in the Chelyabinsk Region. The methodological basis of the research was formed by the subject-activity and resource approaches. To determine the level of resilience and the characteristics of coping behavior among convicts with disabilities, a comprehensive psycho-diagnostic examination was carried out, which made it possible to identify differences in the levels of resilience, in coping strategies of convicted persons with disabilities and convicts without disabilities, the relationship between the level of resilience of convicted persons with disabilities and their coping behavior, targets of psychological impact. The practical significance of the work lies in the possibility of developing a psycho-correctional program aimed at the harmonious and viable development of the personality of convicted persons with disabilities. Key words: resilience, coping strategies, coping behavior, disabled convicts.
Variability of the interplanetary magnetic field as a driver of electromagnetic induction in Mercury’s interior
Authors: Zomerdijk-Russell Sophia , Masters Adam , Heyner Daniel
Published: July 2021

Mercury’s magnetosphere is a unique and dynamic system, primarily due to the proximity of the planet to the Sun and its small size. Interactions between solar wind and embedded Interplanetary Magnetic Field (IMF) and the dayside Hermean magnetosphere drive an electric current on the system’s magnetopause boundary. So far, electromagnetic induction due to magnetopause motion in response to changing external pressure has been used to constrain Mercury’s iron core size. Here we assess the impact a changing IMF direction has on the Hermean magnetopause currents, and the resulting inducing magnetic field. Observations made by MESSENGER during subsolar magnetopause boundary crossings in the first ‘hot season’, are used to demonstrate the importance of the IMF direction to Mercury’s magnetopause currents. Our 16 boundary crossings show that introduction of external IMFs change the magnetopause current direction by 10° to 100°, compared to the case where only the internal planetary field is considered. Analytical modelling was used to fill in the bigger picture and suggests for an east-west reversal of the IMF, typical of the heliospheric current sheet sweeping over Mercury’s magnetosphere, the inducing field at Mercury’s surface caused by the resulting magnetopause current dynamics is on the order of 10% of the global planetary field. These results suggest that IMF variability alone has an appreciable effect on Mercury’s magnetopause current and generates a significant inducing magnetic field around the planet. The arrival of the BepiColombo mission will allow this response to be further explored as a method of probing Mercury’s interior.
Scheme design and key technology verification of Narrow Angle Sensor for small body mission
Authors: Wu Fenzhi , Liang Xiao , Wu Yanpeng , Zhang Yunfang , Zhao Yuan , Dong Chao , Zuo Fuchang , Liu Xingtan , Zhang Chengyu , Zhang Chengyu
Published: July 2021

   In small body exploration mission, the uncertainty of the target characteristics and the special weak gravitational environment put forward higher requirements for the optical autonomous navigation accuracy of the probe and the detection ability of the navigation sensor. Narrow Angel Sensor(Hereinafter referred to as NAS), as the key instrument of China’s first small body exploration mission, has both optical autonomous navigation function and scientific observation ability, and it must give consideration to both near and far, and achieve breakthroughs in dynamic range, detection sensitivity, pointing measurement accuracy, angular resolution and spectral observation ability. The specific performance is as follows: To capture and track Near Earth Asteroids 2016HO3 from tens of thousands of kilometers, NAS is required to have the ability of point target detection, and the detection sensitivity is better than MV10, and  the accuracy of pointing measurement is better than 1 ″. As the probe approaches the target, NAS must be able to clearly image the shape and surface texture of 2016HO3, so as to obtain the motion parameters such as the spin axis and rotation period of the target. In remote sensing and descending stage, the mission requires NAS to be able to carry out global centimeter scale and landing area millimeter scale multi-spectral observation of the target, and optical navigation uses high-resolution images to construct landmark feature library, so as to realize terrain relative navigation; meanwhile, the image is used to provide data support for the scientific research of the target topography, spectral characteristics and surface material composition analysis.

   NAS adopts split design, and the detector part is composed of front door, baffle, focusing optical system, filter wheel, image processing circuit, and motor drive circuit, the algorithm is implemented in the image navigation processing unit. The prototype of the instruments has been developed, and the function and performances such as MTF, detection sensitivity, pointing measurement accuracy etc were verified. The instrument achieved expected design objectives,  and can meet the requirements of optical autonomous navigation and scientific observation for China’s small body exploration mission.
Characterization of NH4-montmorillonite coexisting with NH4Cl salt at different aggregation states. Application to Ceres.
Authors: Munoz-Iglesias Victoria , Fernández-Sampedro Maite , Gil-Lozano Carolina , J. Bonales Laura , Ercilla Herrero Oscar , Valles González María Pilar , Mateo-Martí Eva , Prieto-Ballesteros Olga
Published: July 2021

Ceres, dwarf planet of the main asteroid belt, is considered a relic ocean world since the Dawn mission discovered evidences of aqueous alteration and cryovolcanic activity [1]. Unexpectedly, a variety of ammonium-rich minerals were identified on its surface, including phyllosilicates, carbonates, and chlorides [2]. Although from the Dawn’s VIR spectroscopic data it was not possible to specify the exact type of phyllosilicates observed, montmorillonite is considered a good candidate owing to its ability to incorporate NH4+ in its interlayers [3]. Ammonium-rich phases are usually found at greater distances from the Sun. Hence, the study on their stability at environmental conditions relevant to Ceres’ interior and of its regolith can help elucidate certain ambiguities concerning the provenance of its precursor materials.In this study, it was investigated the changes in the spectroscopic signatures of the clay mineral montmorillonite after (a) being immersed in ammonium chloride aqueous solution and, subsequently, (b) washed with deionized water. After each treatment, samples were submitted to different environmental conditions relevant to the surface of Ceres. For one experiment, they were frozen overnight at 193 K, and then subjected to 10-5 bar for up to 4 days in a Telstar Cryodos lyophilizer. For the other, they were placed inside the Planetary Atmospheres and Surfaces Chamber (PASC) [4] for 1 day at 100 K and 5.10-8 bar. The combination of different techniques, i.e., Raman and IR spectroscopies, XRD, and SEM/EDX, assisted the assignment of the bands to each particular molecule. In this regard, the signatures of the mineral external surface were distinguished from the interlayered NH4+ cations. The degree of compaction of the samples resulted crucial on their stability and spectroscopic response, being stiff smectites more resistant to low temperatures and vacuum conditions. In ground clay minerals, a decrease in the basal space with a redshift of the interlayered NH4+ IR band was measured after just 1 day of being exposed to vacuum conditions.AcknowledgmentsThis work was supported by the Spanish MINECO projects ESP2017-89053-C2-1-P and PID2019-107442RB-C32, and the AEI project MDM‐2017‐0737 Unidad de Excelencia “María de Maeztu”.References[1] De Sanctis et al.,  Space Sci. Rev. 216, 60, 2020[2] Raponi et al., Icarus 320, 83,  2019[3] Borden and Giese, Clays Clay Miner. 49, 444, 2001[4] Mateo-Marti et al., Life 9, 72, 2019
Peeking inside the Black Box: Interpreting Deep Learning Models for Exoplanet Atmospheric Retrievals
Authors: Yip Kai Hou , Changeat Quentin , Nikolaou Nikolaos , Morvan Mario , Edwards Billy , Waldmann Ingo , Tinetti Giovanna
Published: July 2021

Deep learning algorithms are growing in popularity in the field of exoplanetary science due to their ability to model highly non-linear relations and solve interesting problems in a data-driven manner. Several works have attempted to perform fast retrievals of atmospheric parameters with the use of machine learning algorithms like deep neural networks (DNNs). Yet, despite their high predictive power, DNNs are also infamous for being 'black boxes'. It is their apparent lack of explainability that makes the astrophysics community reluctant to adopt them. What are their predictions based on? How confident should we be in them? When are they wrong and how wrong can they be? In this work, we present a number of general evaluation methodologies that can be applied to any trained model and answer questions like these. In particular, we train three different popular DNN architectures to retrieve atmospheric parameters from exoplanet spectra and show that all three achieve good predictive performance. We then present an extensive analysis of the predictions of DNNs, which can inform us - among other things - of the credibility limits for atmospheric parameters for a given instrument and model. Finally, we perform a perturbation-based sensitivity analysis to identify to which features of the spectrum the outcome of the retrieval is most sensitive. We conclude that for different molecules, the wavelength ranges to which the DNN's predictions are most sensitive, indeed coincide with their characteristic absorption regions. The methodologies presented in this work help to improve the evaluation of DNNs and to grant interpretability to their predictions.
Where were the molecules of life made?
Authors: Jheeta Sohan
Published: July 2021

It is believed that some of the necessary organic molecules may have been formed in specific areas of space (namely dark molecular clouds, eg Horsehead nebula) and delivered on to the Earth during the early heavy bombardment period of its history, approximately 4.3-4.0 billion years ago. These organic molecules may have played a pivotal role in the formation of life on Earth. In addition, it is believed that life on Earth was formed within a very short geological time frame of only 200-300 million years. So, it is not unreasonable to suppose that these molecules were initially made in space which in effect could be, metaphorically speaking, a huge chemical laboratory.
The research (drawn from my own experimental astrochemistry) highlighted during this oral presentation focuses on the formation of molecules under a variety of simulated space conditions (eg different temperatures, levels of radiation energies and types of impinging radiations). There are two sorts of chemistry that take place in space, solid and gas phase, and although only 25% of the chemistry in space occurs in the solid phase, this will be the focus of my oral presentation.
The 2009 Wesley impact: Asteroidal or Cometary?
Authors: Sinclair James , Orton Glenn , Krishnamoorty Meera , Fletcher Leigh , Hora Joseph , Lisse Carey , Palotai Csaba , Hayward Thomas
Published: July 2021

We present Earth-based observations of Jupiter from 1994 and 2009, which respectively capture the effects on Jupiter’s atmosphere by the impacts of Comet D/Shoemaker-Levy 9 (SL9) and the impact by an unknown object whose visible impression on Jupiter’s appearance was discovered by Anthony Wesley.  Previous studies have suggested the 2009 impactor was by an asteroid on the basis of differences in Jupiter’s atmospheric response compared to the 1994 impact by SL9.  These differences include detections of 9.1-μm silicate features in the 2009 impact site (Orton et al., 2010, Icarus 211, 587-602) and the fact the 2009 debris field shrank faster (Hammel et al., 2010, ApJL 715, L150-L154), both of which suggest the 2009 impactor was more rocky/refractory in composition.  However, Schenk et al. 2004 (Jupiter: The Planet, Satellites and Magnetosphere, Bagenal, Dowling, McKinnon, 427-456) state that comets are orders of magnitude more likely to impact Jupiter than asteroids since Jupiter should have cleared its orbit a long time ago. Thus, either (1) the 2009 impact was caused by an asteroid and therefore a statistical fluke, (2) Jupiter-Family Comets (JFCs) are a highly heterogeneous population, with some containing rocky/refractory interiors hidden from remote-sensing, or (3) there is a population of asteroids among bodies classified as JFCs. In order to explore these hypotheses, we performed a comparative spectral re-analysis of broadband imaging and low-resolution spectra measured during/after the 1994 and 2009 impacts. The comparison used consistent procedures for reduction and calibration of the data, atmospheric models, radiative-transfer software and spectroscopic line data in order to facilitate direct comparisons between 1994 and 2009 events.  
Io’s dry body shaped by atmospheric instability
Authors: Mousis Olivier , Marcq Emmanuel , Aguichine Artyom , Leblanc François , Mandt Kathleen , Schneeberger Antoine , Turbet Martin
Published: July 2021

One of the outstanding questions regarding the architecture of the Galilean moons system is the nature of the processes that shaped its density gradient, which results from the fact that Ganymede and Callisto share an ice-to-rock ratio close to unity while Io and Europa are heavily depleted in volatiles. Two categories of scenarios, gathered in two distinct phases of moons formation and evolution, have been proposed to account for this density gradient in the literature: either the building blocks of the two innermost moons Io and Europa have been depleted in volatiles during their migration in the hot part of the Jovian circumplanetary disk [1-3], or they initially accreted ice-rich building blocks in a colder environment. In this case, their primitive oceans would have mostly vanished via hydrodynamic escape due to the high accretional energy [4].Figure 1.Thickness of Io’s primitive atmosphere (in units of satellite radius) expressed as a function of pressure (in units of surface pressure) for several temperatures.Here, we investigate the possibility that Io also accreted from water-rich building blocks and that its hydrosphere vanished because of hydrostatic instability, i.e. when the gravity at a given height is insufficient to retain gas. Io’s putative primordial atmosphere would be either situated atop of a magma mantle, or a coexisting liquid ocean, depending on the surface temperature and pressure. To do so, we use the atmosphere model elaborated by [5,6] in which the properties of a 1D spherical atmosphere of water are generated by integrating the thermodynamic profiles bottom to top. The model takes as inputs the satellite’s mass and radius, as well as the thermodynamic conditions at its bottom. Figure 1 represents the atmosphere thickness as a function of surface pressure and temperature. It shows that atmospheric thicknesses higher than 10 Io’s radii are reached for surface temperatures equal or higher than 1250 K, indicating that such H2O-dominated atmospheres would be gravitationally unstable at those temperatures. Such high temperatures needed at the base of the atmosphere to favor hydrostatic instabilitycould result from the combination of accretional heating and heating generated by greenhouse effect. If effective, this mechanism would naturally explain why Io is devoid in volatiles without the need of invoking pre-accretional formation scenarios. [1] Canup, R.M. & Ward, W.R. 2002, AJ, 124, 3404. doi:10.1086/344684[2] Mousis, O. & Gautier, D. 2004, PSS, 52, 361. doi:10.1016/j.pss.2003.06.004[3] Ronnet, T., Mousis, O., & Vernazza, P. 2017, ApJ, 845, 92. doi:10.3847/1538-4357/aa80e6[4] Bierson, C.J. & Nimmo, F. 2020, ApJL, 897, L43. doi:10.3847/2041-8213/aba11a[5] Marcq, E., Salvador, A., Massol, H., et al. 2017, JGR (Planets), 122, 1539. doi:10.1002/2016JE005224[6] Marcq, E. 2012, JGR (Planets), 117, E01001. doi:10.1029/2011JE003912  
INAF Online Lab: can hands-on, educational laboratories be online?
Authors: Duras Federica , Giacomini Livia , Mantovani Giulia
Published: July 2021

INAF Online Lab is the name of the project born within EduINAF (the online magazine of the Italian Institute of Astrophysics) during the Covid-19 pandemic and the subsequent rearrangement of the outreach and teaching activities normally carried out in person. These online laboratories are an example of how to virtually take by the hand those same young people with whom only a year ago it was possible, and indeed natural, to interact live. From their schools or homes, the students are guided through the activity by an experienced operator, and take on the role of astronomers while building, observing, learning and wondering about the great mysteries of space. The four online laboratories currently active have been optimized to be perfectly usable during science festivals in an interactive way and at practically no cost.Throughout the presentation, we will describe the project and its possible applications and evolutions, with some examples to be shown to the audience.
Mars ionosphere during two consecutive solar minima
Authors: Sanchez-Cano Beatriz , Lester Mark , Cartacci Marco , Orosei Roberto , Witasse Olivier , Blelly Pierre-Louis , Kofman Wlodek
Published: July 2021

Mars Express has been exploring Mars since late 2003 giving us fascinating views of the red planet as well as unique science insights. The long-life of Mars Express is an asset in order to understand the long-term evolution of the atmosphere of Mars, and in particular, of the ionosphere and upper atmosphere. Currently, we have about 16 years of ionospheric observations at Mars, which cover near two cycles of solar activity. This is the first time that such a long time series observations can be investigated in other planet rather than Earth.  In particular, this work focuses on Mars’ ionospheric behaviour during two consecutive solar minima (23/24 and 24/25) using the same dataset. We use the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) on board Mars Express to investigate the total electron content behaviour of the whole atmosphere in relation to key parameters, such as the solar flux, solar illumination, dust storms and Sun-Mars distance. The topside variability of the ionosphere is also investigated through variations in the neutral scale height, and results are supported by ionospheric modelling. The main goal of this study is to investigate whether the ionosphere during the recent solar minimum 24/25 was similar (and to which degree) to the ionosphere at solar minimum 23/24, which was characterised by a pronounced reduction of both the topside and bottomside regions.
Sulfuric acid vapor and sulfur dioxide in the atmosphere of Venus as observed by the Venus Express Radio Science Experiment VeRa
Authors: Oschlisniok Janusz , Häusler Bernd , Pätzold Martin , Tellmann Silvia , Bird Michael
Published: July 2021

The main cloud deck within Venus' atmosphere, which covers the entire planet between approx. 50 and 70 km altitude, is believed to consist mostly of liquid sulfuric acid. The temperature below the main clouds is high enough to evaporate the H2SO4 droplets into gaseous sulfuric acid forming a haze layer which extends to altitudes as deep as 35 km. Gaseous sulfuric acid in Venus’ lower atmosphere is responsible for a strong absorption of radio waves as seen in Mariner, Pioneer Venus, Magellan and Venera radio science observations. Radio wave absorption measurements can be used to derive the amount of H2SO4 in Venus’ atmosphere. The radio science experiment VeRa onboard Venus Express probed the atmosphere of Venus between 2006 and 2014 with radio signals at 13 cm (S-band) and 3.6 cm (X-band) wavelengths. The orbit of the Venus Express spacecraft allowed to sound the atmosphere over a wide range of latitudes and local times providing a global picture of the sulfuric acid vapor distribution. We present the global H2SO4(g) distribution derived from the X-band radio signal attenuation for the time of the entire Venus Express mission. The observation is compared with results obtained from a 2-D transport model. The VeRa observations were additionally used to estimate the abundance of SO2 near the cloud bottom. The global distribution of SO2 at these altitudes is presented and compared with results obtained from other experiments. Eight years of VEX observation allow to study the long-term evolution of H2SO4 and SO2. The latter is presented for the northern polar region.
PRISMA: an Italian network for the recovery of freshly fallen meteorites
Authors: Barghini Dario , Carbognani Albino , Di Carlo Matteo , Di Martino Mario , Gardiol Daniele , Pratesi Giovanni , Riva Walter , Stirpe Giovanna Maria , Volpicelli Cosimo Antonio ,   PRISMA team
Published: July 2021

PRISMA is the Italian fireball network dedicated to the observation of bright meteors. It is active since 2016 and formed a collaboration involving more than 60 institutes, being coordinated by INAF, the Italian National Institute for Astrophysics. PRISMA is also a member of the European network FRIPON. To date, the network counts more than 60 all-sky detectors and has observed more than 2000 bright meteor, four of them being meteorite-dropping fireballs with a predicted strewn-field over the Italian territory. On 04/01/2020, two meteorite pieces were recovered near Cavezzo (MO) in the predicted area just three days after the fall. This was the first recovery of this type in Italy. However, due to the morphology of the two fragments, other meteorites pieces are yet to be found. More recently, on 15/03/2021, a similar event was observed in the skies of southern Italy, near Isernia. Searches for the meteorite are still ongoing, involving the local people and volunteers. In addition, two more meteorite-dropping fireballs were observed, in 2017 and 2018, for which a reliable strewn-field is available. We will report on the current status of the network operations.
NEOROCKS characterization programme of near-Earth asteroids previously observed with radar
Authors: de León Julia , Licandro Javier , Popescu Marcel , Medeiros Hissa , Morate David , Pinilla-Alonso Noemi , Perez-Toledo Fabricio , Planetary Radar Team* Arecibo ,   NEOROCKS Team
Published: July 2021

Introduction. The NEO Rapid Observation, Characterization and Key Simulations (NEOROCKS) project is funded (2020-2022) through the H2020 European Commission programme to improve our knowledge on near-Earth objects by connecting expertise in performing small body astronomical observations and the related modelling needed to derive their dynamical and physical properties. The Instituto de Astrofísica de Canarias (IAC), and in particular members of the Solar System Group, participate in the NEOROCKS project and currently lead one specific task: to collect observational data, mainly in the visible and near-infrared wavelength regions, of NEAs that have been observed in the past using the Arecibo Planetary Radar. In this work we present preliminary results, focusing on those targets having high signal-to-noise ratio radar data.Observations. Our observations include spectroscopy, color photometry and lightcurves. They are performed using the facilities located at the Observatorios de Canarias (OOCC), that include the El Teide Observatory in the island of Tenerife and the El Roque de los Muchachos Observatory in the island of La Palma. Visible and near-infrared spectra are mainly obtained using the 10.4-m Gran Telescopio de Canarias (GTC) and its visible (OSIRIS) and near-infrared (EMIR) spectrographs. We also use the ALFOSC spectrograph at the 2.5-m Nordic Optical Telescope (NOT). Visible color photometry is obtained using the MuSCAT2 instrument at the 1.5-m Telescopio Carlos Sánchez (TCS). The setup allows to obtain simultaneous imaging in the g, r, i, and zsvisible bands. Time-series photometry in the visible is obtained using several telescopes, including the 46-cm TAR2, 80-cm IAC-80, and 1-m Jacobus Kapteyn Telescope (JKT).Results. Spectra in the visible and/or the near-infrared wavelengths, as well as color photometry in the visible, are used to taxonomically classify the targets and to infer their composition (Fig 1). In the case of having no albedo measurements for one object, we can also use the taxonomy to have an estimation of the albedo based on the spectral class, and therefore determine the size of the asteroid. Lightcurves are used to both get the asteroid rotational period and, together with radar data, to obtain the shape and the spin axis orientation of the target (Fig. 2). In this way, a full characterization can be obtained for every asteroid observed within this program. Acknowledgements. This project has received funding from the European Union’s Horizon 2020 research and innovation programme  under grant agreement No 870403.
Detection of OH at the evening terminator of the ultra-hot Jupiter WASP-76b
Authors: Landman Rico , Sánchez-López Alejandro , Mollière Paul , Kesseli Aurora , Louca Amy , Snellen Ignas
Published: July 2021

Ultra-hot Jupiters have dayside temperatures similar to those of M-dwarfs. While molecular absorption from the hydroxyl radical (OH) is easily observed in near-infrared spectra of M-dwarfs, it is often not considered when studying the atmospheres of (ultra-)hot Jupiters. We use high-resolution spectroscopic near-infrared observations of a transit of WASP-76b obtained using CARMENES to assess the presence of OH. After validating the OH line list, we generate model transit spectra of WASP-76b with petitRADTRANS. The data are corrected for telluric contamination and cross-correlated with the model spectra. After combining all cross-correlation functions from the transit, a detection map is constructed. OH is detected in the atmosphere of WASP-76b with a signal-to-noise ratio of 6.1. From a Markov Chain Monte Carlo retrieval we obtain Kp=234 km/s and a blueshift of 13.9 km/s. Considering the fast spin-rotation of the planet, the OH signal is best explained with the signal mainly originating from the evening terminator and the presence of a strong day- to nightside wind. The signal appears to be broad, with a full width at half maximum of 16.2 km/s. The retrieval results in a weak constraint on the temperature of 2420-3150 K at the pressure of the OH signal. Our results demonstrate that OH is readily observable in the transit spectra of ultra-hot Jupiters. Studying this molecule can give new insights in the molecular dissociation processes in the atmospheres of such planets.
Mass-Radius relationships of small, highly irradiated exoplanets with small water mass fractions
Authors: Vivien Hugo , Aguichine Artem , Mousis Olivier , Deleuil Magali , Marcq Emmanuel
Published: July 2021

This work aims to determine the mass-radius rela-tionships of highly irradiated (500< Tirr
Analogue experiments for the detection of bacterial biosignatures in ice grains relevant to ocean worlds
Authors: Bönigk Janine , Pavlista Miriam , Klenner Fabian , Napoleoni Maryse , Hillier Jon K. , Khawaja Nozair , Dannemann Marie , Klauck Eberhard , Abel Bernd , Olsson-Francis Karen , Postberg Frank
Published: July 2021

The identification of biosignatures on extraterrestrial ocean worlds is key to the search for life on these bodies. Saturn’s icy moon Enceladus, and possibly Jupiter’s moon Europa, eject plumes containing gas and ice grains formed from subsurface salty water into space [1,2,3,4]. The emitted ice grains can be analyzed by impact ionization mass spectrometers, such as the Cosmic Dust Analyzer (CDA) onboard the earlier Cassini-Huygens mission [5] or the Surface Dust Analyzer (SUDA) onboard the upcoming Europa Clipper mission [6] rendering the ocean’s composition accessible for analysis during spacecraft flybys [7]. CDA data collected in the Saturnian system revealed that Enceladus’ ocean is salty [8] and contains a variety of organic material, including complex macromolecules [9] and low mass volatile compounds [10]. These low mass compounds can potentially act as amino acid precursors and could be capable of interacting within or near Enceladus’ hydrothermal vent systems [11], or Enceladus’ porous rocky core [12]. These findings enhance Enceladus’ relevance as a habitable environment potentially able to support microbial life in its subsurface ocean. However, biosignatures have not yet been identified in extraterrestrial environments.The Laser Induced Liquid Beam Ion Desorption (LILBID) experiment is proven to accurately reproduce impact ionization mass spectra of ice grains recorded in space [13]. Previous analogue experiments using this setup have shown that amino acids, fatty acids and peptides could successfully be detected in simulated ocean world scenarios [14,15]. The next step is to investigate whether the characteristic mass spectral fingerprints of bacterial life forms, if enclosed in ice grains, could also be detected and identified by SUDA-type instruments.We therefore conducted high sensitivity LILBID experiments on extracts of two bacteria, Sphingopyxis alaskensis (S.alaskensis) and Escherichia coli (E.coli), to simulate their characteristic spectral features in cationic and anionic impact ionization mass spectra. E. coli is a well-studied model bacterium, and S. alaskensis is a model oligotroph, abundant in marine environments. The predictable, small size of S. alaskensis (
Updated Ganymede Mosaic from Voyager and Galileo observations
Authors: Kersten Elke , Zubarev Anatoly E. , Roatsch Thomas , Matz Klaus-Dieter
Published: July 2021

AbstractIn preparation of the JUICE mission with the primary target Ganymede [1] we generated a new controlled version of the global Ganymede image mosaic using a combination of Voyager 1 and 2 and Galileo images. Baseline for this work was the new 3D control point network from Zubarev et al., 2016 [2], which uses the best available images from both missions and led to new position and pointing of the images.Introduction
Voyager 1 and Voyager 2 encountered Jupiter in 1979. They took 490 Narrow Angle Camera (NAC) and Wide Angle Camera (WAC) images of Ganymede’s surface with pixel scales from 470 m/pxl down to 20 km/pxl. Galileo entered orbit around Jupiter in 1995 and flew by Ganymede 15 times to acquire 149 images (
Main-belt debris on comet-like orbits
Authors: Shober Patrick , Sansom Eleanor , Bland Phil , Devillepoix Hadrien , Towner Martin , Cupak Martin , Howie Robert , Hartig Benjamin , Anderson Seamus
Published: July 2021

Understanding the tension between the dynamical and physical characteristics of solar system debris has been a goal of astronomers and planetary scientists for a long time. This study considered a large (>1400) dataset of orbits gathered from six years of fireball observations observed by the Desert Fireball Network. We focused on the meteoroids we detected originating from short-period comet orbits (2 < TJ < 3). We examined how durable they were as they went through the atmosphere and their orbital evolution over the previous ten thousand years. Our results show that almost all of the meteoroids we see in this size range are sourced from the main belt, not the Jupiter-family comet population. The fact that we do not see these objects shows that genetically cometary material in the centimeter size range does not last long in the inner solar system. Even when meteor shower debris is taken into account, the majority of material at centimeter to meter-scales on comet-like orbits is from the main belt.We worked with inclusive criteria to be considered cometary in origin. To be classified as cometary, a meteoroid must be at least a Type II according to the PE criterion and have a >50% probability of originating from an unstable orbit over the previous 10 kyrs. Of the 50 sporadic comet-like fireballs observed by the DFN since 2014, only 2 fulfilled this criterion (figure below). Using a Markov Chain Monte Carlo to draw samples from the posterior distribution, we found that sporadic JFC-like meteoroids in NEO space is 94.2% ± 3.2% from the main belt when considering an uninformed prior. This demonstrates that cometary debris has physical lifetimes in near-Earth space less than the decoherence lifetimes for a stream (
Cometary Activity Begins at Kuiper Belt Distances: Evidence from C/2017 K2
Authors: Jewitt David , Kim Yoonyoung , Mutchler Max , Agarwal Jessica , Li Jing , Weaver Harold
Published: July 2021

We discuss the development of activity in the extraordinary, distant long-period comet C/2017 K2 over the heliocentric distance range 9 < rH < 16 AU.  C/2017 K2 is an incoming long-period comet with a period so long (~ 3 Myr) that no heat from the previous perihelion can be retained; we can be sure that the observed mass-loss is driven by the current insolation and not by a thermal lag.  The comet is characterized by a steady-state coma of sub-millimeter and larger particles ejected at low (4 m/s) velocity, filling a roughly spheroidal coma with a characteristic scale of 80,000 km.  In a fixed, co-moving volume around the nucleus we find that the scattering cross-section of the coma, C, is related to the heliocentric distance by a power law, C ~ rH-s, with heliocentric index s = 1.14+/-0.05. This dependence is significantly weaker than the rH-2, variation of the insolation as a result of two effects.  These are, first, the heliocentric dependence of the dust velocity and, second, a lag effect due to very slow-moving particles ejected long before the observations were taken.   A Monte Carlo model of the photometry shows that dust production beginning at rH ~ 35 AU is needed to match the measured heliocentric index, with only a slight dependence on the particle size distribution.  Dust mass loss rates at 10 AU are of order dM/dt ~ 103 a1 kg/s, where 0.1 < a1 < 1 is the effective particle radius expressed in millimeters.The expulsion of submillimeter and larger grains, beginning at Kuiper belt distances, is likely the result of the sublimation of near-surface supervolatile ice (probably CO, as suggested by the recent detection of this molecule at 6.7 AU; Yang et al. Ap. J. Letters, in press). Water ice is involatile over the observed distance range and even the energy and gas release triggered by the crystallization of amorphous ice, if present, cannot produce activity at 35 AU.  Comet C/2017 K2 will reach perihelion near Mars' orbit in December 2022.   This work is described in D. Jewitt, Y. Kim. M. Mutchler, J. Agarwal, J. Li and H. Weaver (2021).  Astronomical Journal, 161:188 (11pp) 
Magnetic topology at Venus: new insights to the Venus plasma environment
Authors: Xu Shaosui , Frahm Rudy , Ma Yingjuan , Mitchell David , Luhmann Janet
Published: July 2021

Venus lacks significant intrinsic magnetic fields and thus its atmosphere and ionosphere interact directly with the solar wind flow and magnetic fields. Interplanetary magnetic fields (IMF) can penetrate into the ionosphere when the upstream solar wind dynamic is stronger than the ionospheric plasma pressure. Magnetic topology can be inferred at Venus if it is defined as the magnetic connectivity to the collisional atmosphere/ionosphere, rather than connectivity to the planet’s surface. Utilizing electron and magnetic field measurements from the Venus Express mission, this study provides the first characterization of magnetic topology at Venus by examining the pitch angle and energy distribution of superthermal (> ~1 eV) electrons. More specifically, the presence of loss cones in electron pitch angle distributions infers the connectivity to the nightside collisional atmosphere and the presence of ionospheric photoelectrons (identified from electron energy distributions) indicates the connectivity to the dayside collisional ionosphere. We show case examples of various magnetic topology types at Venus, including the most expected draped IMF, open field lines connected to the nightside atmosphere, open field lines connected to the dayside ionosphere, and, most surprisingly, cross-terminator closed field lines. More interestingly, during one of the ionospheric hole events identified by Collinson et al. [2014, JGRA], we discover not only the expected open magnetic topology but also a field-aligned potential drop, which has implications for its formation mechanism. The characterization of magnetic connectivity could provide new insights into many important topics on Venus, such as planetary ion outflow, energetic electron precipitation (possible auroral emission), and the formation mechanism of Venusian ionospheric holes.
Atmospheric Entry Probes for in situ Exploration of the Ice Giant Planets
Authors: Atkinson David H. , Mousis Olivier J. , Hofstadter Mark , Atreya Sushil K.
Published: July 2021

Understanding the formation and evolution of the solar system and the formation of the giant planets is constrained by inherent limitations in the capabilities of remote sensing. In situ exploration of planetary atmospheres provides key measurements not possible from remote observations, remarkably demonstrated at Jupiter by the Galileo probe, where key measurements included the determination of noble gas abundances and the precise measurement of the Jupiter helium mixing ratio. In this paper, we describe the primary scientific goals to be addressed by future in situ exploration of the ice giants Uranus and Neptune, placing in situ explorations of the gas giants, including the Galileo probe and a future Saturn probe, into a broader solar system context. An ice giant atmospheric entry probe reaching 10 bars would provide insight into both the formation history of the solar system and the giant planets, and the structure and composition of, and physical processes at play within ice giant atmospheres. An entry probe as an element of a future ice giant flagship mission would descend under parachute to measure the abundances and isotopic ratios of the noble gases, D/H in H2 and 13C/12C, and the thermal structure and dynamics from the upper atmosphere down to the deepest region from which the probe is able to return data, perhaps 10-20 bars or more. Probe data would be returned to Earth using a Carrier Relay Spacecraft as a relay station. The relay spacecraft, particularly if it is an orbiter with a suite of remote sensing instruments, can significantly enhance the science return from the probe; remote sensing provides the global context from which to understand the probe's local measurements of weather and cloud properties. One or more small atmospheric probes could represent a significant ESA contribution to a future NASA New Frontiers or Flagship Ice Giant mission.

 
Synergistic studies enhanced through data assimilation: combining multiple retrievals with a Mars Global Circulation Model
Authors: Holmes James , Lewis Stephen , Patel Manish , Streeter Paul , Rajendran Kylash
Published: July 2021

The wealth of observations now available from multiple spacecraft in orbit around Mars and rovers/landers on the surface provides information on several aspects of the atmosphere, although they are restricted in space and time. Most of the observational datasets are largely complementary, so an efficient method to combine them in a physically consistent way will lead to more constrained studies of the evolution of the global martian atmosphere. Data assimilation is one such method, combining multiple retrievals with a Mars Global Circulation Model (GCM) while accounting for errors in both sources of information and producing an optimal representation of the evolving martian surface and atmosphere. Data assimilation is a powerful tool in that multiple parameters each observed independently by different instruments (e.g. water vapour, ozone, carbon monoxide, dust opacity, temperature) are all realistically constrained and physically consistent at the same time, and unobserved parameters can also be influenced by assimilated data (e.g. water vapour assimilation will impact on the water ice distribution). It also allows for study of atmospheric features that change significantly between observations and identifying processes that lead to the observed changes. 

Data assimilation studies are prevalent on Earth and are becoming more mainstream for Mars, with several different Mars GCMs now capable of assimilating retrievals using different assimilation schemes. The Open University (OU) ExoMars modelling group Mars GCM has been combined with several retrieval datasets via data assimilation to study features of the ozone, carbon monoxide, water and dust cycles alongside dynamical features such as the polar vortices, surface warming during a global dust storm and planetary waves. OpenMARS (Open access to Mars Assimilated Remote Soundings), a publicly available global reanalysis dataset from 1999-2015, was also created using the OU assimilation system. 

This talk will give a brief overview of the benefits and limitations of data assimilation for Mars, and will demonstrate how combining retrievals of different atmospheric parameters with a Mars GCM via data assimilation leads to a better constrained analysis of the martian atmosphere than is possible with retrievals or GCMs alone. 
Simulating haze radiative feedback in general circulation models of hot Jupiters
Authors: Steinrueck Maria , Koskinen Tommi , Lavvas Panayotis , Zhang Xi , Tan Xianyu
Published: July 2021

Photochemically produced hazes provide a possible explanation for aerosol features in the transmission spectra of many hot Jupiters, especially those with relatively low equilibrium temperatures. Recent simulations of photochemical hazes as passive tracers in a 3D general circulation model demonstrate that the distribution of hazes can be highly inhomogeneous, with horizontal abundance variations of over an order of magnitude. At the same time, one-dimensional radiative transfer models show that absorption and scattering by hazes can change the atmospheric temperature profile by several hundred Kelvin. The additional heating and cooling have the potential to significantly affect atmospheric circulation. In this talk, we present new GCM simulations of hot Jupiter HD 189733b that include radiative feedback from hazes. A focus will be on changes in the atmospheric temperature structure and circulation. We will then compare the 3D haze distribution from previous simulations with radiatively passive hazes to the new haze distribution in simulations that include haze radiative feedback. Finally, we predict transit spectra based on the simulations and compare them to observations.
An update on the Solar System Treks Mosaic Pipeline: public server and new mosaic products
Authors: Curtis Aaron , Lethcoe Heather , Law Emily , Day Brian
Published: July 2021

Solar System Treks (https://trek.nasa.gov) allows you to exploring the solar system in your web browser. Many of the digital terrain models and orthoimage mosaics viewable on Solar System Treks were created using a custom kubernetes-based pipeline, which we released open source in 2020 as the Solar System Treks Mosaic Pipeline (SSTMP). SSTMP manages workflows based on open-source applications including USGS ISIS and Ames Stereo Pipeline. It contains several templates for mosaic workflows to create stereo and imagery mosaics from Lunar Reconaissance Orbiter Narrow Angle Camera imagery, and is eventually will be expanded to include workflow templates to process imagery from a wide range of orbiters on all of the bodies that Solar System Treks supports (e.g. Mars, Venus, Ceres, Vesta, Bennu, Europa, etc.)

Until recently, using SSTMP required installation on a Kubernetes cluster, which is a significant barrier to entry for many potential users. In response to this, we are creating a public-facing SSTMP server which allows turnkey mosaic creation. The user only needs to go to the website and select the area of interest, and SSTMP does the rest: determining the best imagery, downloading and ingesting it, computing stereo reconstruction, merging and formatting the result. Here we present the status of this tool and a demonstration.

Additionally, we present new imagery products recently produced by SSTMP, including some experimental stereo reconstructions in the south polar region of the moon.
Infographics and illustrations for planetary science
Authors: Utreras José , Roche Paul
Published: July 2021

Communicating our knowledge in astronomy is our duty with society, and this should be done in a format that is appealing and comprehensive. This last part is a difficult task. According to theory, verbal information and pictorial information are processed in different cognitive systems. Graphics that are not related to verbal information, or that do not take into account prior knowledge of individuals may interfere with mental model construction. Creating scientific illustrations for learners needs to tackle three points: (1) accurate scientific knowledge (2) appealing design (3) learner experience.   Illustrations and infographics have the benefit of simplifying problems, can show us abstract representations, or can tell stories about discoveries, making them a flexible tool to take into account learner experience. That has led Europlanet to develop illustrated material that can be easily shared online or be used in public talks or school activities.During the last months, we have been creating illustrations for different topics of planetary science: moons, icy objects, and an illustrated guide to Mars. We want to show our work and progress to our peers, get feedback, and hopefully show to the scientific community the benefits of using illustrations and art to communicate with a broader audience. Specifically, we want to present part of the illustrated guide to Mars through our poster, showing that not only we can show information about Mars, we can also tell a bit about the history of the exploration of the red planet.The style of this material has already been tested successfully on social media platforms. We will translate the infographics into multiple languages starting with English and Spanish.Here are some of the illustrations that we have created. 

  
Exploring Disequilibrium Chemistry in Exoplanet Atmospheres with a Grid of Pseudo-2D Photochemical Models
Authors: Baeyens Robin , Decin Leen , Carone Ludmila , Venot Olivia , Agúndez Marcelino , Mollière Paul
Published: July 2021

Irradiated exoplanet atmospheres, with their hot day sides and eternally dark night sides, are intrinsically three-dimensional and highly dynamical. Vigourous atmospheric motions are expected to mix the atmosphere, reducing potential chemical variations with longitude. Day-side photochemistry, on the other hand, would enhance those variations. Both mixing and photochemistry drive the atmospheric chemistry out of equilibrium, and, as of yet, it is unclear to what degree both processes influence the composition of different exoplanet atmospheres.We will present results from a grid of atmospheric disequilibrium chemistry models, incorporating vertical mixing, horizontal advection and photochemical reactions. Our grid spans a wide range of planetary temperatures (400 K – 2600 K), surface gravities, and rotation rates, so we will highlight the role that dynamical mixing and photochemistry play in each corner of the parameter space. We further focus on the compositional differences between the day- and night-side hemispheres that may arise, or be washed away, by disequilibrium chemistry processes. Finally, the influence of these processes on observations, such as transmission spectra, will be discussed. This work provides valuable constraints on the importance of disequilibrium chemistry, and the expected chemical diversity of exoplanets, with regards to upcoming space missions.