bluuebunny/crossref_metadata_2025 huggingface dataset:
Mapping the regional tectonic asset of the Discovery quadrangle of Mercury
Authors: Galluzzi Valentina , Ferranti Luigi , Giacomini Lorenza , Palumbo Pasquale
Published: July 2021

The Discovery quadrangle of Mercury (H-11) located in the area between 22.5°S–65°S and 270°E–360°E encompasses structures of paramount importance for understanding Mercury’s tectonics. The quadrangle is named after Discovery Rupes, a NE-SW trending lobate scarp, which is one of the longest and highest on Mercury (600 km in length and 2 km high). By examining the existing maps of this area (Trask and Dzurisin, 1984; Byrne et al., 2014), several other oblique trending structures are visible. More mapping detail could be achieved by using the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) Mercury Dual Imaging System (MDIS) imagery.We aim at mapping the structures of H-11 at high-resolution by using MESSENGER/MDIS basemaps, in order to understand its regional tectonic history by following the work done in the Victoria quadrangle (H-2) (Galluzzi et al., 2019). Differently from H-2, located in the same longitudinal range but at opposite latitudes, this area lacks in N-S trending scarps, such as the Victoria-Endeavour-Antoniadi fault system, which dominates the northern hemisphere structural framework. The existing tectonic theories predict either an isotropic pattern of faults (global contraction) or an ordered distribution and orientation of faults (tidal despinning) for Mercury. If we expect that the existing tectonic patterns were governed by only one of the two processes or both together, it is difficult to understand how such different trends formed within these two complementary areas. The structural study done for H-2 reveals that the geochemical discontinuities present in Mercury’s crust may have guided and influenced the trend and kinematics of faults in that area (Galluzzi et al., 2019). In particular, the high-magnesium region seems to be associated with fault systems that either follow its boundary or are located within it. These fault systems show distinct kinematics and trends. The south-eastern border of the HMR is located within H-11. Hence, with this study, we aim at complementing the previous one to better describe the tectonics linked to the presence of the HMR. Furthermore, this geostructural map will complement the future geomorphological map of the area and will be part of the 1:3M quadrangle geological map series which are being prepared in view of the BepiColombo mission (Galluzzi, 2019). Acknowledgments: We gratefully acknowledge funding from the Italian Space Agency (ASI) under ASI-INAF agreement 2017-47-H.0.Byrne et al. (2014). Nature Geoscience, 7(4), 301-307.Galluzzi, V. (2019). In: Planetary Cartography and GIS, Springer, Cham, 207-218.Galluzzi et al. (2019). Journal of Geophysical Research: Planets, 124(10), 2543-2562.Trask and Dzurisin (1984). USGS, IMAP 1658.
Realistic visualization of solar system small bodies using Blender ray tracing software
Authors: Penttilä Antti , Palos Mario F. , Kohout Tomas
Published: July 2021

Physically realistic simulated images of small bodies are needed, for example, when planning for space mission operations and testing for performance of imaging instruments on board. With smaller bodies (asteroids, comets), the geometry of the body and the photometric properties of the surface might not be known in detail before the mission. However, one can use rougher shape models and simulate realistic small-scale surface features such as boulders, craters, and albedo variations. Using this kind of simulated target shape, one can employ ray tracing software such as Blender (https://www.blender.org/) and create physically realistic models of irradiances received by a camera on a spacecraft with given position.
We have developed a Python/Blender-based software package (https://bitbucket.org/mariofpalos/asteroid-image-generator/) that is targeted to simulate the performance of the ASPECT hyperspectral camera onboard the MILANI CubeSat on ESA Hera mission. We also seek to develop the package to be used with the MIRMIS hyperspectral camera onboard the ESA Comet Interceptor mission. The package can both be used to produce the simulated image of the target in given observing geometry, and the same image when taking into account the optics throughput and the sensitivity of the detector. Planetary photometric functions such as Lommel-Seeliger and ROLO models are programmed as Blender shaders for realistic output.  Therefore, the tool can be used to optimize the mission operations from the imaging point of view, and to verify the performance of the imaging instrument in the planned conditions.

Figure: An example image of rough-scale geometric model of the asteroid (101955) Bennu with simulated procedural small-scale details on the surface. The visualization is done in Blender using Lommel-Seeliger photometric shader.
Modeling asteroid shapes using BNAO Rozhen photometric data in combination with sparse data
Authors: Apostolovska Gordana , Vchkova Bebekovska Elena , Borisov Galin , Kostov Andon , Donchev Zahary
Published: July 2021

Our work aims to demonstrate how the use of our dense lightcurves in combination with sparse data from diverse sources will affect the results for obtaining the sidereal period, shape models, and ecliptic pole solution for a chosen asteroid.Photometric observations of minor planets are traditional at the Bulgarian National Astronomical observatory (BNAO) Rozhen. They started with photoelectric observations in 1991, and later have been continued as CCD photometric observations on all three telescopes: 2m Ritchey-Chretién-Coudé, 50cm/70cm, and 60cm Cassegrain. We hope that the new 1.5 m robotic telescope planned to be operational next year will be also partly devoted to the study of minor planets.Our target, 339 Dorothea, is a main-belt asteroid, a large member of the Eos dynamical family. For the last 8 years, between 2013 and 2021, the asteroid 339 Dorothea was observed at BNAO Rozhen during six apparitions and several dense lightcurve were obtained. We used these dense photometric data in lightcurve inversion method and reconstruct the model of the asteroid, determining its sidereal period, shape, and pole orientation. Afterward, using sparse data from the AstDys database with an accuracy of 0.01 mag in combination with the obtained dense data, new trials for calculating and improving the physical characteristics of the asteroid 339 Dorothea were made.Unlike very low photometric accuracy in ground-based sparse photometry, space missions have provided astronomers with sparse photometry with extremely high accuracy, for example, the ESA GAIA mission. The NEOWISE mission has observations only for a limited number of asteroids. Fortunately, we were able to find some sparse data for our target and use this accurate photometry in combination with our dense lightcurves for the reconstruction of the asteroid spin state and shape model.Due to bad weather conditions and limited allocation of observing time at the BNAO Rozhen dedicated to our project, we have at our disposal full and partial dense lightcurves obtained for several more asteroids in few different apparitions. Combining these dense data with ground-based or space mission sparse data will contribute to enlarging the database of asteroids with known physical characteristics. Enriching the number of asteroids with known physical parameters would provide more data for future statistical analysis and could help in answering the questions for the evolution of our Solar System. 
The 3.1 μm absorption feature on asteroids (24) Themis and (65) Cybele is not due to surface water ice
Authors: O'Rourke Laurence , Müller Thomas G. , Biver Nicolas , Bockelée-Morvan Dominique , Hasegawa Sunao , Valtchanov Ivan , Küppers Michael , Fornasier Sonia , Campins Humberto , Fujiwara Hideaki , Teyessier David , Lim Tanya
Published: July 2021

Previous research on Asteroids (24) Themis and (65) Cybele have shown the presence of an absorption feature at 3.1 μm reported to be directly linked to surface water ice. We searched for water vapor escaping from these asteroids with the Herschel Space Observatory HIFI (Heterodyne Instrument for the Far Infrared) Instrument. While no H2O line emission was detected, we obtained sensitive 3σ water production rate upper limits of Q(H2O)< 4.1×1026 molecules s−1 for Themis and Q(H2O)
From atmospheric to exoplanet formation retrievals
Authors: Mollière Paul , Molyarova Tamara , Bitsch Bertram , Eistrup Christian , Burn Remo , Nasedkin Evert , Henning Thomas , Semenov Dmitry , Mordasini Christoph , Kreidberg Laura , Schlecker Martin , Lacour Sylvestre , Nowak Mathias
Published: July 2021

With new and upcoming observing facilities (JWST and the ELTs), the exoplanet community is poised to precisely measure the chemical inventory of exoplanet atmospheres. This will allow, for the first time, to start investigating whether one of the greatest promises of atmospheric characterization studies holds up: inverting the atmospheric composition to infer the planet formation history encoded in it. In my talk, I will show how such measurements allow to run so-called formation retrievals, which constrain a planet’s formation history using its atmospheric abundances in a Bayesian retrieval framework. I will demonstrate how simple and popular models for the composition of the protoplanetary disk and planet formation could lead to interesting insights when applied in formation retrievals. At the same time, I will discuss how such assumptions are too strongly simplified for making the exoplanet atmosphere — formation connection in practice, and what the most pressing theoretical challenges are. Achieving this connection will be a formidable and interdisciplinary challenge, but the exciting exoplanet observations that lie ahead will allow the community to tackle it in earnest.
Global upper-atmospheric heating at Jupiter by the recirculation of auroral energy
Authors: O'Donoghue James , Moore Luke , Bhakyapaibul Tanapat , Melin Henrik , Stallard Tom , Connerney Jack , Tao Chihiro
Published: July 2021

Jupiter's upper atmosphere is significantly hotter than expected based on the amount of solar heating it receives. This temperature discrepency is known as the 'energy crisis' due to it's nearly 50-year duration and the fact it also occurs at Saturn, Uranus and Neptune. At Jupiter, magnetosphere-ionosphere coupling gives rise to intense auroral emissions and enormous energy deposition in the magnetic polar regions, so it was presumed long ago that redistribution of this energy could heat the rest of the planet. However, most global circulation models have difficulty redistributing auroral energy globally due to the strong Coriolis forces and ion drag on this rapidly rotating planet. Consequently, other possible heat sources have continued to be studied, such as heating by gravity and acoustic waves emanating from the lower atmosphere. Each global heating mechanism would imprint a unique signature on global temperature gradients, thus revealing the dominant heat source, but these gradients have not been determined due a lack of planet-wide, high-resolution data. The last global map of Jovian upper-atmospheric temperatures was produced using ground-based data taken in 1993, in which the region between 45o latitude (north & south) and the poles was represented by just 2 pixels. As a result, those maps did not (or could not) show a clear temperature gradient, and furthermore, they even showed regions of hot atmosphere near the equator, supporting the idea of an equatorial heat source, e.g. gravity and/or acoustic wave heating. Therefore observationally and from a modeling perspective, a concensus has not been reached to date. Here we report new infrared spectroscopy of Jupiter's major upper-atmospheric ion H3+, with a spatial resolution of 2o longitude and latitude extending from pole to equator, capable of tracing the global temperature gradients. We find that temperatures decrease steadily from the auroral polar regions to the equator. Further, during a period of enhanced activity possibly driven by a solar wind compression, a high-temperature planetary-scale structure was observed which may be propagating from the aurora. These observations indicate that Jupiter's upper atmosphere is predominantly heated via the redistribution of auroral energy, and therefore that Coriolis forces and ion drag are observably overcome.
3D simulations of dust trapping in gaseous vortices
Authors: Rendon Restrepo Steven , Barge Pierre
Published: July 2021

    Large scale vortices are thought to be natural outcomes of hydrodynamic instabilities in protoplanetary disks, as for instance the Rossby Wave Instability [1] or Baroclinic instability. Analytical and numerical studies showed that they can be long-lived and catalyze efficiently dust material concentration [2], [3] what encourages to think they could play a role in protoplanetary-disk evolution and planetesimal formation. Their presence in the outer regions of circumstellar disks is possibly betrayed by recent observations of lopsided structures with ALMA and VLT [4], [5].    We present our latest results of two-phase 3D numerical simulations in which the solid particles are embedded in the gas and described as a second pressureless fluid.  The goal is to discuss the sedimentation of the dust phase in the protoplanetary disk midplane, and the dust trapping mechanism induced by 3D vortices. We will also address the question if 3D vortices are more stable to the streaming instability than 2D vortices.Figure 1. Left : Three 3D vortices generated by the Rossby Wave instability. Right : Same as left but two vortices merged after few orbital periods[1] Lovelace, R. V. E., Li, H., Colgate, S. A., & Nelson, A. F. 1999, ApJ, 513, 805[2] Barge, P. & Sommeria, J. 1995, A&A, 295, L1[3] Raettig N, Klahr H Lyra W (2015), ApJ804[4] Tsukagoshi, T., Muto, T., Nomura, H., et al. 2019, ApJ, 878, L8[5] Dong, R., Liu, S.-y., Eisner, J., et al. 2018, ApJ, 860, 124
Soapbox Science Brussels: an outreach platform for the promotion of Women in Sciences in Belgium
Authors: Bingen Christine , Pham Lê Binh San , Lamort Lucie , Lefever Karolien , Piccialli Arianna , Yseboodt Marie
Published: July 2021

In June 2021, the second edition of Soapbox Science takes place in Brussels. Soapbox Science is a public outreach platform that was initiated in London, UK in 2011 to promote women in science, and that was spread worldwide since then. Between 2011 and 2018, 40 cities hosted the initiative in not less than 8 countries over 4 continents, and in 2020, despite the pandemic, 56 events were organized in 14 countries around the world.In 2019, the idea to endorse the organisation of a Soapbox Science event in Brussels was germinating in the head of a small group of scientists from two Belgian Federal Scientific Institutes. After about 20 months of exploratory work and of addressing the challenges posed by the COVID pandemic, the first Belgian event took place in fall 2020, not in the centre of Brussels as initially planned, but as a virtual event live-streamed via YouTube and Facebook. The second edition of Soapbox Science Brussels will take place end June 2021, and the organisation is now much better prepared to adapt the format of the event (online or in the heart of Brussels following the standard format) to the latest developments of the regulations of the pandemic.In this communication, we present the development of the Soapbox Science initiative in Belgium. We describe the motivations, challenges, issues and opportunities encountered throughout the process, and how Soapbox Science gradually takes its place in the Belgian context of the promotion of women in sciences.
Studying Cassini’s photoelectrons during a series of solar eclipses in Saturn, using data from Cassini's Langmuir Probe
Authors: Xystouris Georgios , Arridge Christopher Stephen , Morooka Michiko , Wahlund Jan-Erik
Published: July 2021

The Langmuir Probe (LP) onboard Cassini was one of the three experiments that could measure the cold inner magnetospheric plasma, along with the Radio and Plasma Waves Science (RPWS) and the Cassini Plasma Spectrometer (CAPS). While the century-old LP theory looks quite straight-forward, in reality things are much more complicated.The operation of the LP is quite simple: by applying positive bias voltages, the probe attracts the electrons and repels the ions of the surrounding plasma. From the resulting current-voltage curve characteristics of the ambient electrons can be estimated, i.e. density and temperature. When negative bias voltages are applied to the probe the characteristics of the ambient ions can be estimated, i.e. density, temperature, and mass.Though the LP operation and interpretation are quite simple and straightforward, there are assumptions made and therefore the theoretical models may not always reflect the actual plasma conditions in Saturn’s magnetosphere. For this study we are focused on the effect of the photoelectrons, i.e. electrons that are generated by the incident sunlight on Cassini’s surfaces, which are difficult to be observed and corrected for in a laboratory plasma.We developed a robust algorithm that identifies the transitions of the LP in and out of shadow caused by the Saturn and its rings. The LP data inside and outside the eclipses are compared using the algorithm developed. In this presentation we will discuss the impact of the photoelectron generation from the spacecraft surfaces to the LP current-voltage curves, and understand the variations of the measured plasma density connected with the photoelectrons.
Bayesian Spectroscopic Characterization of Directly Imaged Planets and Brown Dwarfs and Implications for Ultracool Model Atmospheres
Authors: Zhang Zhoujian , Liu Michael , Marley Mark , Line Michael , Best William
Published: July 2021

Spectroscopic characterization of imaged exoplanets and brown dwarfs is essential for understanding their atmospheres, formation, and evolution, but such work is challenged by the unavoidably simplified model atmospheres needed to interpret spectra. While most previous work has focused on single or at most a few objects, comparing a large collection of spectra to models can uncover trends in data-model inconsistencies needed to improve model predictions, thereby leading to robust properties from exoplanet and brown dwarf spectra. Therefore, we are conducting a systematic analysis of a valuable but underutilized resource: the numerous high-quality spectra of (directly imaged and free-floating) exoplanets and brown dwarfs already accumulated by the community. Focusing on the cool-temperature end, we have constructed a Bayesian modeling framework using the new Sonora-Bobcat model atmospheres and have applied it to study near-infrared low-resolution spectra of >50 late-T imaged planets and brown dwarfs (≈600-1200K, ≈10-70 MJup) and infer their physical properties (effective temperature, surface gravity, metallicity, radii, mass). By virtue of having such a large sample of high-quality spectra, our analysis identifies the systematic offsets between observed and model spectra as a function of wavelength and physical properties to pinpoint specific shortcomings in model predictions. We have also found that the spectroscopically inferred metallicities, ages, and masses of our sample all considerably deviate from expectations, suggesting the physical and chemical assumptions made within these models need to be improved to fully interpret data. Our work has established a systematic validation of cloudless model atmospheres to date and we discuss extending such analysis to wider temperature and wavelength (e.g., JWST) ranges, as well as finding new planetary-mass and brown dwarf benchmarks, in order to validate ultracool model atmospheres over larger parameter space.
Realizing the Potential of JWST High Contrast Imaging with Coronagraphic Phase-Retrieval
Authors: Ygouf Marie , Beichman Charles A , Rocha Graça M , Green Joseph J , Jeffrey B Jewell , Roudier Gael M , Greenbaum Alexandra , Leisenring Jarron , Girard Julien , Pueyo Laurent , Perrin Marshall , Meyer Michael , De Furio Matthew , Uyama Taichi
Published: July 2021

  The James Webb Space Telescope (JWST) will probe circumstellar environments at an unprecedented sensitivity. However, the performance of high-contrast imaging instruments is limited by the residual light from the star at close separations (
The Open Polar Cap of Rotating Magnetospheres
Authors: Zhang Binzheng
Published: July 2021

The classic Dungey cycle plays an essential role in understanding the dynamics of the terrestrial magnetosphere. However, its direct applicability to planetary magnetospheres such as Jupiter is limited, especially when the planetary rotation is much faster than the Earth. We use a series of numerical experiments to show the transition of the terrestrial magnetosphere from a classic Dungey cycle, convection-dominated system to rotation-dominated configurations. The numerical experiments use the Earth's magnetosphere-ionosphere system as a testbed, with modified rotation speed to increase the influence of planetary rotation over solar wind driving, characterized by the ratio between the solar wind merging potential and the polar cap rotation potential. Results show that when the rotation potential of the polar magnetosphere becomes comparable to the merging potential of the solar wind, the classic Dungey cycle is modified by azimuthal transport of magnetic flux, resulting in a more closed polar magnetosphere with a crescent-shaped open flux region in the ionosphere. These numerical experiments provide a theoretical framework for understanding the fundamentals of magnetospheric physics, which is potentially applicable to the Saturn, Jupiter, and exo-planetary systems.
Examining the emission and transmission spectra of WASP-79b with retrieval 
Authors: Bieger Michelle , Changeat Quentin
Published: July 2021

Retrieval tools provide a way of determining an exoplanet atmosphere's temperature structure and composition with an observed planetary spectrum, working backwards to determine the chemistry and temperature by iteratively comparing synthetic spectra that have been constructed via a forward model to the observed spectra and determining a best-fit result (Barstow and Heng, 2020). This talk will be presenting the emission and reanalysed transmission spectrum and retrieval analysis of WASP-79b, an inflated hot Jupiter first detected by Smalley et al. (2012). Previous transmission spectra of WASP-79b has been analysed in Sozten et al. (2020), Skaf et al. (2020), and Rathcke et al. (2021); all studies agreeing on detections of H2O with various confidence levels, with the latter finding moderate evidence of an H- bound-free opacity compared to iron hydride abundance found by the other studies. Using the publicly available \verb+Iraclis+ data analysis pipeline and the Bayesian atmospheric retrieval framework TauREx 3, we will be adding to the global picture of this planet by examining the Hubble Space Telescope emission spectra as captured by the Wide Field Camera 3 G141 grism (PI: David Sing, proposal ID: 14767). 
Community Access to CHEOPS
Authors: Isaak Kate , Lüftinger Theresa
Published: July 2021

Launched on 18 December 2019, CHEOPS (CHaracterising ExOPlanet Satellite) is the first exoplanet mission dedicated to the search for transits of exoplanets by means of ultrahigh precision photometry of bright stars already known to host planets. It is the first S-(small) class mission in ESA’s Cosmic Vision 2015-2025, and a partnership between Switzerland and ESA, with important contributions from 10 other member states.CHEOPS will provide the unique capability of determining accurate radii for a subset of planets in the super-Earth to Neptune mass range, for which masses have already been estimated from ground- based spectroscopic surveys. It will also provide precision radii for new planets discovered by ground- and space-based transit surveys, including TESS. By combining known masses with CHEOPS sizes, it will be possible to determine accurate densities for these smaller planets, providing key insight into their composition and internal structure. By identifying transiting exoplanets with high potential for in-depth characterisation – e.g. those that are potentially rocky and have thin atmospheres - CHEOPS will also provide prime targets for future instruments suited to the spectroscopic characterisation of exoplanetary atmospheres.In this poster we detail how the Community can access CHEOPS, with emphasis on the ESA-run Guest Observers Programme and the Annual Announcement of Opportunity for observing time Year 3 of CHEOPS, which is foreseen to come out in Quarter 4 2021.
The many roles of quantum tunnelling in chemical and biological evolution
Authors: Trixler Frank
Published: July 2021

Tunnelling is a non-trivial quantum phenomenon which becomes effective at scales of around one nanometer and below. It enables elementary particles and atoms to negotiate an energetic barrier without having sufficient energy to overcome it. That seemingly paradoxical phenomenon might seem to be an exotic process only important for particle physics and quantum physical applications such as the Tunnel Diode or Scanning Tunnelling Microscopy.This review discusses why quantum tunnelling is of vital importance for prebiotic chemistry and molecular biology and how physical and chemical processes which are essential for the chemical and biological evolution can be traced directly back to the effect of quantum tunnelling. These processes include the chemical evolution within the cold interstellar medium and within stars, prebiotic chemistry in the subsurface and atmosphere of planetary bodies, the rise and persistence of habitable conditions via insolation and geothermal heat and the function of complex biomolecules. The contribution provides a highly multidisciplinary view on quantum tunnelling in the context of the research on the origin and evolution of life and shows that tunnelling makes significant complexification in molecular and biological evolution possible by providing different sources of constant energy flux over a long period of time, enables synthesis pathways for astrochemical reactions which would otherwise not occur, and enables or influences specific functions of biomolecular nanomachines that maintain the process of life.ReferenceTrixler. Quantum Tunneling to the Origin and Evolution of Life. Curr. Org. Chem. 17(16), 1758-1770 (2013). DOI: 10.2174/13852728113179990083
Instruments Operations, Science and Innovation in Expedition Support: EuroMoonMars-Etna campaign 202
Authors: Reilly Hannah , Foing Bernard , Brady Gary , Mohan Chirayu , McGrath Kevin , Lakomiec Patrycja , Ehreiser Anouk , De Palma Gaia , Schlarmann Leander , Wedler Armin , Schmitz Nicole , Pagano Isabella
Published: July 2021

An expedition EMM-Etna to simulate the Lunar and Martian volcanic and soil environment will be carried out at Mount.Etna’s Cratere del Laghetto in Sicily, near Catania Italy by the EuroMoonMars TUDublin and LEAPS ExoMars groups. This scouting campaign intends to train in using instruments to be used on MoonMars landers and rovers, with a perspective of ARCHES DLR telerobotics campaign to be conducted in June 2022, and in preparation for ExoMars rover instruments (PANCAM, CLUPI and spectrometers) science and operations.   Figure 1: Lunar Lander and REMMI Rover for Sample AnalysisThe aim of this EMM-Etna expedition is to investigate and analyse the terrain with the use of different scientific instruments. The topography of the landscape will be photographed using a 360° panoramic camera and drone; it will be processed, and a 3D model developed. The terrain will also be investigated using the REMMI Rover, the abilities of the rover to operate and transport equipment will be monitored. This will further develop the knowledge available of the terrain and help future expeditions to identify different landmarks. The use of a Radio Jove Antenna will permit the team to monitor transmissions from both the Sun and Jupiter. This will allow different cosmic events or changes in the celestial objects to be studied and explored. On site a selection of different samples will also be collected and examined using the REMMI Rover. An Ocean Optics UV-Vis-NIR spectrometer will a be operated  in order to evaluate the existence of biological compounds and substances within these samples and in the area itself. It is key to understand the molecular makeup of one’s surroundings when in an unknown environment. By analysing samples collected, spectroscopy can be used to identify and determine a diagnostic for each substance. This process will be monitored by a Logitech camera to ensure it is carried put correctly. A selection of photographs will be captured of each sample using a portable optical microscope. This will allow an in-depth analysis of the microscopic structure of each collected sample. The use of all of the instruments mentioned above is key in the investigation and research into the Moon and Martian-like volcanic environment that is Mount Etna.We would also like to thank Prof I. Pagano's team from the University of Catania and Dr A.Wedler's team from DLR Deutsches Zentrum für Luft- und Raumfahrt for their support in organising this expedition.
Rover testing for lunar science and innovation
Authors: Mohan Chirayu , Foing Bernard , Charasse Mael-Alois
Published: July 2021

REMMI,  Rover for EuroMoonMars Investigations has been built at EMMIHS campaign in HI-SEAS Hawaii in 2019 and teleoperated locally and from The Netherlands. For EuroMoonMars  2021 projects, a number of scientific experiments were carried out with the REMMI rover. These experiments were based primarily on teleoperation of the REMMI rover and its mobility system. The rover’s mobility system is based on a continuous track system. It was discovered through experimentation that these tracks are suitable for a number of environments but unsuitable for others. When testing was done in the Analog Astronaut Training Center in Poland, the rover showed that it had difficulty getting a grip on metal surfaces. However, through testing in other outdoor facilities, it was observed that the rover had greater grip on sandy surfaces, grass surfaces and rocks. There was, however, a number of issues with these surfaces. On grass and rock surfaces, small debris would often interfere with the gears of the rover and would prevent movement. The solution to this would be to have a covering to shield the mobility system from both smaller debris and in future, lunar regolith. The rover also had issues with large slopes and inclines. Overall, it was discovered that the REMMI rover was more of a support rover than an exploration rover.The REMMI rover also has a camera on it to allow for remote operation. This camera unlocks a number of future possibilities. Firstly, it will allow the rover to take pictures of samples and areas which the astronaut may want to collect or explore. This is a great feature for the astronaut as they will not have to waste oxygen and resources during an EVA searching for samples. The REMMI rover’s camera also unlocks the possibility to use artificial intelligence to recognise different features of the environment. Similar to self-driving cars, it would theoretically be possible to allow the rover to recognise features of the landscape which would show dangerous terrain for the rover or perhaps a new area to discover. The possibilities will be further tested in July 2021 on Mt Etna, Italy. Acknowledgements: The authors would like to thank the Analog Astronaut Training Center and Dr. Kołodziejczyk for allowing the REMMI rover to be tested in their facilities and for their support throughout. The authors would also like to thank ILEWG EuroMoonMars for providing the REMMI rover for testing.Figure 1: REMMI rover showing continuous track system and manoeuvrable camera. 
Science and innovation from the Moon: Radio antenna precursor observations
Authors: Brady Gary , Foing Bernard
Published: July 2021

In coordination with ILEWG EuroMoonMars, a number of radio antenna tests have been carried out and analysed for solar observations. The instrument used for this data collection is the radio Jove, connected to a single dipole antenna at a set height. Data is recorded using a software program known as Radio-SkyPipe and the audio from the observations is analysed in person by the operator and recorded using livestreaming platforms for later analysis. Noise is a major factor while trying to operate this device, as such, a quiet location and fine tuning is essential for isolating the favoured frequency range. Solar activity plays a major role in the success of the device. While carrying out solar observations, the sought after transmissions are from solar bursts and flares. These transmissions can be very difficult to capture as a result of low solar activity, up-time of the device and external noise.  The device has been tested in a number of locations in Leiden, Netherlands and will be later tested on on lunar volcanic ash analogue in Cratere di Laghetto,  in Mount Etna, Catania, Sicily.  As a result of observations to date, a solar burst has been isolated for later analysis.  In the near future, the device will be used for Jupiter observations. This data will be analysed and compared to data which has been obtained through solar observations in order to see the changes between the two transmissions. We shall learn from this EMM-Etna field tests to prepare the analysis of DLR-ESA ARCHES Etna 2022 tele-robotic campaign that will deploy with rovers an array of 4 radio VLF antennas, among a number of rover science and technical tasks. Acknowledgements: we thank Chirayu Mohan, Kevin McGrath and Hannah Reilly for their help setting up the device. As well as Fabian Mulder for his hospitality in Leiden Innovation CenterPLNT & "The Field" and the EuroMoonMars ExoMars team along with the ARCHES Etna team for providing support in Sicily. Fig. Single dipole set-up for solar, jovian and cosmic observations
Retrieving the transmission spectrum of HD 209458b usingCHOCOLATE: a new Chromatic Doppler Tomography technique
Authors: Esparza-Borges Emma , Oshagh Mahmoud , Casasayas-Barris Nuria , Pallé Enric
Published: July 2021

Multi-band photometric transit observations or low resolution spectroscopy (spectro-photometry) are normally used to retrieve the broadband transmission spectra of transiting exoplanets in order to assess the chemical composition of their atmospheres. In this work, we present an alternative approach for recovering the broadband transmission spectra using chromatic Doppler Tomography. To validate the method and examine its performance, we used new observational data obtained with the ESPRESSO instruments to retrieve the  transmission spectra of the archetypal hot Jupiter HD209458b. Our findings indicate that the recovered transmission spectrum is in good agreement with the results presented in previous studies, which used different methodologies to extract the spectrum.
Planetary Science in Ethiopia
Authors: Belay Tessema Solomon
Published: July 2021

Planetary Science in Ethiopia research has been emerged in Ethiopia based on the establishment of Entoto Observatory and Research Center (EORC) as well as special commencement of special graduate in three specialized fields such as (astronomy and astrophysics, space science, remote sensing and Geodesy). The installation of the twining optical telescope and ratification of national space policy has opened many opportunities to focus of planetary science research and training in Ethiopia.  Ethiopia has progressed in research, training, and technology and infrastructure development in planetary science, space technology and astronomy. This paper will focus on planetary science and related activities, current development and future prospects.
The Pacific Ocean heat engine
Authors: Jones Roger N. , Ricketts James H.
Published: July 2021

Abstract. Historical warming forms a sequence of steady-state regimes punctuated by abrupt shifts. These changes are regulated by a heat engine spanning the tropical Pacific Ocean teleconnected to a broader climate network. The eastern-central Pacific maintains steady-state conditions, delivering heat to the Western Pacific warm pool. They form a heat pump with heat moving from the cold to the warm reservoir, sustained by kinetic energy. The two reservoirs exchange heat on a range of timescales, with oscillatory behaviour that intensifies under forcing. The heat engine is part of a network of oscillations and circulation interacting on a range of timescales. The process is self-regulating: steady-state regimes persist until they become unstable due to an over- or under-supply of heat for dissipation, shifting warmer or cooler to a new stable state. Pre-industrial climate was in free mode, characterised by a loosely-coupled ocean-atmosphere with limited circulation, moving into forced mode in the latter 20th century, characterised by tighter coupling and stronger circulation through the tropical Pacific with more active teleconnections globally. Continued forcing produces a stepladder-like pattern of warming. Most shifts coincide with phase changes in decadal oscillations, switching from slower to faster modes of dissipation. El Niño events combine with regime shifts to propagate heat from the oceans to land and from the tropics to higher latitudes. The most recent shift commenced in the warm pool in December 2012, ending the so-called hiatus (1997–2013), global mean surface temperatures warming abruptly by ~0.25 °C in 2014–15.
Hydrological response of a peri-urban catchment exploiting conventional and unconventional rainfall observations: the case study of Lambro catchment
Authors: Cazzaniga Greta , De Michele Carlo , D'Amico Michele , Deidda Cristina , Ghezzi Antonio , Nebuloni Roberto
Published: July 2021

Abstract. Commercial Microwave Links (CMLs) can be used as opportunistic and unconventional rainfall sensors by converting the received signal level into path-averaged rainfall intensity. Since in meteorology and hydrology the reliable reconstruction of the rainfall spatial distribution is still a challenging issue, there is a wide-spread interest in integrating the precipitation estimates gathered by the ubiquitous CMLs with the conventional rainfall sensors, i.e. rain gauges (RGs) and weather radars. Here we investigate the potential of a dense CML network, for the estimation of river discharges via a semi-distributed hydrological model. The analysis is conducted on Lambro, a peri-urban catchment located in northern Italy and covered by 50 links. A two-level comparison is made between CML- and RG-based outcomes, relying on 12 storm/flood events. First, rainfall data are spatially interpolated and assessed in a set of significant points of the catchment area. Rainfall depth values obtained from CMLs are definitively comparable with direct RG measurements, except for the spells of persistent light rain, due to limited sensitivity of CMLs caused by the coarse quantization step of raw power data. Moreover, it is showed that, when changing the type of rainfall input, a new calibration of model parameters is required. In fact, after the re-calibration of model parameters, CML-driven outputs performances are comparable with RG-driven ones, confirming that the exploitation of a CML network may lead to benefit in hydrological modelling.
Wave dispersion and dissipation in landfast ice: comparison of observations against models
Authors: Voermans Joey J. , Liu Qingxiang , Marchenko Aleksey , Rabault Jean , Filchuk Kirill , Ryzhov Ivan , Heil Petra , Waseda Takuji , Nose Takehiko , Kodaira Tsubasa , Li Jingkai , Babanin Alexander V.
Published: July 2021

Abstract. Observations of wave dissipation and dispersion in sea ice are a necessity for the development and validation of wave-ice interaction models. As the composition of the ice layer can be extremely complex, most models treat the ice layer as a continuum with effective, rather than independently measurable, properties. While this provides opportunities to fit the model to observations, it also obscures our understanding of the wave-ice interactive processes, particularly, it hinders our ability to identify under which environmental conditions these processes are of significance. Here, we aimed to reduce the number of free variables available by studying wave dissipation in landfast ice. That is, in continuous sea ice, such as landfast ice, the effective properties of the continuum ice layer should revert to the material properties of the ice. We present observations of wave dispersion and dissipation from a field experiment on landfast ice in the Arctic and Antarctic. Independent laboratory measurements were performed on sea ice cores from a neighbouring fjord in the Arctic to estimate the ice viscosity. Results show that the dispersion of waves in landfast ice is well described by theory of a thin elastic plate and such observations could provide an estimate of the elastic modulus of the ice. Observations of wave dissipation in landfast ice are about an order of magnitude larger than in ice floes and broken ice. Comparison of our observations against models suggests that wave dissipation is attributed to the viscous dissipation within the ice layer for short waves only, whereas turbulence generated through the interactions between the ice and waves is the most likely process for the dissipation of wave energy for long periods. The separation between short and long waves in this context is expected to be determined by the ice thickness through its influence on the lengthening of short waves. Further studies are required to measure turbulence underneath the ice independently of observations of wave attenuation to confirm our interpretation of the results.
Changes in Supraglacial Lakes on George VI Ice Shelf, Antarctic Peninsula: 1973–2020
Authors: Barnes Thomas James , Leeson Amber Alexandra , McMillan Malcolm , Verjans Vincent , Carter Jeremy , Kittel Christoph
Published: July 2021

Abstract. High densities of supraglacial lakes have been associated with ice shelf instability and collapse. 2020 was a record melt year on George VI ice shelf with ~12 % of its northernmost portion being covered by lakes. We use 208 Sentinel-2 and Landsat-1-8 satellite images from the past 47 years, together with climate data and firn modelling, to assess the long-term presence of lakes on George VI, thus placing 2020 within a historical context. We find that the ~12 % lake coverage observed in 2020 is not unprecedented and similar to previous high lake years; events of similar magnitude occurred at least five times previously. Secondly, we find lake coverage is controlled by a combination of melting, accumulation, firn air content and firn build-up strong melting alone does not entail high lake coverage. Instead, while melting contributes positively to lake formation, we find accumulation to act as a limiting factor on the formation of lakes in response to melt, introducing new frozen material to the surface, thus cooling and storing meltwater. We find accumulation’s ability to limit melt to be further enhanced by its build-up, increasing available firn air content, and thus meltwater storage capacity. Our findings are supported by comparative analysis, showing years such as 1989 to have 55 % less melt, but similar lake coverage to 2020. Finally, we find that climate projections suggest future temperature increases, but steady snowfall in this region. Thus, in future there will be a greater propensity for higher lake densities on North George VI ice shelf, and associated risk of instability.
COMPREHENSIVE ASSESSMENT OF PHYSICAL DEVELOPMENT YOUNG SCHOOL CHILDREN
Authors: Shkhaeva D.M. , Ulendeev E.M. , Ramazanov D.R. , Tsechoeva M.A. , Kuznetsova M.V.
Published: July 2021

In the context of modern study, the problem of preserving and strengthening the health of schoolchildren is becoming more and more urgent. The article presents information on the physical development of children of primary school age. The analysis of deviations in the physical development of younger schoolchildren will help from the first year of study to properly organize preventive measures to improve their health.
INTERRELATION AND CONTRADICTIONS OF THE PROCESSES OF GLOBALIZATION AND CULTURAL GLOBALIZATION
Authors: Gappasova A.G. , Sadykova T.M. , Stamova R.D.
Published: July 2021

Cultural globalization, as well as the process of globalization itself, is a highly ambiguous and highly contradictory phenomenon that has both positive and negative features and consequences. Since the globalization of culture is a direct and inevitable consequence of the process of globalization itself, its positive and negative impact on certain cultures is unscientific to consider in isolation from this process. The close relationship between these two phenomena, in which cultural globalization is defined as a whole by the process of globalization as such, obliges us to consider some fundamental aspects, properties of the latter, in order to identify those features of cultural globalization that are objective in the sense that they can neither be prevented nor avoided, nor give any other direction to the processes caused and determined by these features. The article examines the relationship between these two processes and their main contradictions.
Adams, E. (2016). Eileen Adams: agent of change in art, design and environmental education.
Authors: Palacios-Garrido Alfredo
Published: July 2021

Reseña del libro autobiográfico de Eileen Adams
A Failure to Regulate? The Demands and Dilemmas of Tackling Illegal Content and Behaviour on Social Media
Authors: Yar Majid
Published: July 2021

The proliferation and user uptake of social media applications has brought in its wake a growing problem of illegal and harmful interactions and content online. Recent controversy has arisen around issues ranging from the alleged online manipulation of the 2016 US presidential election by Russian hackers and ‘trolls’, to the misuse of users’ Facebook data by the political consulting firm Cambridge Analytica (Hall 2018; Swaine & Bennetts 2018). These recent issues notwithstanding, in the UK context, ongoing concern has focused in particular upon (a) sexually-oriented and abusive content about or directed at children, and (b) content that is racially or religiously hateful, incites violence and promotes or celebrates terrorist violence. Legal innovation has sought to make specific provision for such online offences, and offenders have been subject to prosecution in some widely-publicised cases. Nevertheless, as a whole, the business of regulating (identifying, blocking, removing and reporting) offending content has been left largely to social media providers themselves. This has been sustained by concerns both practical (the amount of public resource that would be required to police social media) and political (concerns about excessive state surveillance and curtailment of free speech in liberal democracies). However, growing evidence about providers’ unwillingness and/or inability to effectively stem the flow of illegal and harmful content has created a crisis for the existing self-regulatory model. Consequently, we now see a range of proposals that would take a much more coercive and punitive stance toward media platforms, so as to compel them into taking more concerted action. Taking the UK as a primary focus, these proposals are considered and assessed, with a view to charting possible future configurations for tackling illegal social media content.