bluuebunny/crossref_metadata_2025 huggingface dataset:
The Martian environment observed by NOMAD on ExoMars Trace Gas Orbiter
Authors: Vandaele Ann Carine , Daerden Frank , Thomas Ian R. , Aoki Shohei , Depiesse Cédric , Erwin Justin , Neary Lori , Piccialli Arianna , Ristic Bojan , Robert Séverine , Trompet Loïc , Viscardy Sébastien , Willame Yannick , Gérard Jean-Claude , Villanueva Geronimo , Mason Jon , Patel Manish , Bellucci Giancarlo , Lopez-Valverde Miguel , Lopez-Moreno Jose-Juan
Published: July 2021

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter has been designed to investigate the composition of Mars' atmosphere, with a particular focus on trace gases, clouds and dust. The instrument probes the ultraviolet and infrared regions covering large parts of the 0.2-4.3 µm spectral range [1,2], with 3 spectral channels: a solar occultation channel (SO – Solar Occultation; 2.3–4.3 μm), a second infrared channel capable of nadir, solar occultation, and limb sounding (LNO – Limb Nadir and solar Occultation; 2.3–3.8 μm), and an ultraviolet/visible channel (UVIS – Ultraviolet and Visible Spectrometer, 200–650 nm). Since its arrival at Mars in April 2018, NOMAD performed solar occultation, nadir and limb observations dedicated to the determination of the composition and structure of the atmosphere.NOMAD has been accumulating data about the Martian atmosphere and its surface since its insertion. We will present some results covering the atmosphere composition including clouds and dust, climatologies of water, carbon monoxide and ozone. We also report on the different discoveries highlighted by the instrument by pointing to a series of contributions to this conference that will present in detail several specific studies, like recent progress in the instrument calibration, the latest CO2 and temperature vertical profiles, studies of aerosol nature and distribution, water vapor profiles and variability, carbon monoxide vertical distribution, dayglow observations; detection of HCl, its vertical profiles and in general advances in the analysis of the spectra recorded by the three channels of NOMAD.References[1] Vandaele, A.C., et al., 2015. Planet. Space Sci. 119, 233-249.[2] Vandaele et al., 2018. Space Sci. Rev., 214:80, doi.org/10.1007/s11214-11018-10517-11212. 
Crust, mantle and core structure of Mars from InSight seismic data
Authors: Khan Amir ,   the InSight team
Published: July 2021

With the deployment of a seismometer on the surface of Mars as part of NASA’s InSight mission,the Seismic Experiment for Interior Structure (SEIS) has been collecting continuous data since early 2019.The primary goal of InSight is to improve our understanding of the internal structure and dynamics of Mars, inparticular crust, mantle, and core. Here we describe constraints on the structure of the mantle of Mars basedon inversion of seismic body wave arrivals from a number of low-frequency marsquakes.We consider 8 of the largest (moment magnitude is estimated to be between 3 and 4) low-frequency events withdominant energy below 1 Hz for which P- and S-waves are identifiable, enabling epicentral distance estimation.The 8 events occur in the distance range 25-75 degrees. Body wave arrivals that include the main P- and S-waves,surface reflections (PP, PPP, SS, SSS), and core reflections (ScS) are picked using a set of complimentary methodsthat allows to check for consistency. The resultant set of differential travel times (PP-P, PPP-P, SS-S,...) aresubsequently inverted for radial profiles of seismic P- and S-wave velocity, core size and mean density, and epicentrallocation of the events. To determine interior structure, we rely on independent methods as a means of assessing therobustness of the results.We present a radial velocity model for the upper mantle of Mars, with implications for the thermo-chemical evolutionof the planet that match a cooling, differentiated body, and a thick lithosphere. Based on the location of the events,we are able to constrain structure to the core-mantle-boundary, including the size of the core and its meandensity that point to large liquid and relatively light core, implying a significant complement of light alloyingelements. Our estimate of the average crustal thickness as seen by all events is compatible with the local crustalthickness at the InSight landing determined from observations of converted phases.
Constraints on water vapor content in the lower atmosphere of Mars
Authors: Knutsen Elise Wright , Montmessin Franck , Lefèvre Franck , Giuranna Marco , Verdier Loic
Published: July 2021

By the utilisation of a novel synergistic approach, we constrain the vertical distribution of water vapor on Mars with nadir-pointing instruments. Water vapor column abundances were retrieved simultaneously from PFS (sensing the thermal infrared range) and SPICAM (sensing the near-infrared range) on Mars Express, yielding distinct yet complementary sensitivity to different parts of the atmospheric column. This approach offers a way to study the vertical partitioning of water, which has remained out of the scope of nadir observations made by single instruments covering a specific spectral range. Here we present a global dataset covering all seasons and latitudes, with measurements taken over 8 Martian years. Special focus is given to the high-latitude regions in spring and summer during the sublimation of the seasonal polar cap. A significant deviance was discovered between the retrieved vertical distribution water vapor, and the predicted profile from the Mars Climate Database, which is used as prior. We also show that by exploiting a synergistic retrieval approach, we obtain more accurate water vapor column abundances compared to when only one instrument is used. The synergistic retrieval has a tendency to obtain a lower total column abundance compared to the prior, albeit with a stronger vertical partitioning. This indicates a more prominent low-altitude layer, with more water vapor contained close to the surface than predicted by models.
Effects of Gravity on Delta Morphology and Stratigraphy
Authors: Braat Lisanne , Lamb Michael
Published: July 2021

Deltas are important landforms in planetary research and exploration because they indicate past fluvial activity, contain a sedimentary-record amenable to study, and have the potential to store past signs of life. As exploration missions are searching for (ancient) biomarkers, deltas are targets of interest. Therefore, it is important to understand the differences between deltas on Earth and Mars, so we can adjust our expectations of the past conditions and stratigraphy that we derive from the visible morphology. Furthermore, enhanced understanding of the effects of gravity can improve our estimations about past flow conditions and the duration of fluvial activity in certain areas. This eventually leads to a better understanding of the fluvial history of Mars and improved selection of target locations with the highest probability of preserved biosignatures.To research the effect of gravity on deltas, we use a 2D hydro-morphodynamic numerical model that simulates the flow of water, transport and deposition of sediment, and the evolution of topography. We use the software Delft3D, developed by Deltares research institute (the Netherlands). This software is typically used for river and coastal systems on Earth, but we adapted the software by identifying all explicit and implicit dependencies on gravity, so it can also be used for deltas on Mars. The model set-up consists of a straight channel flowing into a sloping basin. The inflow channel is 200 m wide and the water depth is 3 to 10 m, depending on the model scenario. This results in discharges of about 1000 to 2500 m3/s. We impose two different grain sizes, namely a coarse fraction, transported as bedload, and a fine fraction, transported in suspension.Our preliminary results show that gravity affects fine sediments stronger than coarse sediments, because of the difference in transport mode. For example, reduced gravity significantly slows down suspended sediment settling, while bedload transport is affected less. We expect that this will result in a different delta stratigraphy. This process is in addition to the effect that gravity has on water and sediment fluxes; lower gravity results in a smaller water discharge, while sediment transport is enhanced, with all else held equal. With our modelling efforts, we aim to further investigate the morphological results of these effects.
Methane’s non-linear effect on climate in a three-dimensional Archean atmosphere
Authors: Eager Jake , Mayne Nathan , Lenton Tim
Published: July 2021

The interaction between reduced gases and the pre-oxygenic photosynthesising microbial population is key to determining the potential methane greenhouse that warmed the Archean. The potential biotic methane flux could have sustained methane concentrations between 100 to 35,000ppm [1]. Looking at the effect of these methane fluxes and concentrations in a 3D atmosphere are crucial to understanding these processes in more detail.Here, I will present results from a state-of-the-art 3D climate model [2] along with a low dimensional biogeochemical model [3], exploring the potential biotic methane fluxes and subsequent concentrations. From this, we can examine the potential climate conditions during the Archean. We have extended a 1D exploration of methane’s diminished greenhouse potential during the Archean [4] by looking at how methane concentrations affect cloud distribution, atmospheric dynamics and the surface temperature.We find that global surface temperature peaks at pCH4 ~100 Pa, with this peak shifting at different CO2 concentrations. Equator-to-pole temperature differences also has a peaked response, with the impact strongly dependant on the CO2 concentration. These changes come about from the balance between the effect of methane and carbon dioxide on atmospheric dynamics. This is due to changes in the heating structure of the atmosphere, which also affects the cloud distribution.[1] Kharecha, Kasting & Siefert (2005) Geobiology 3, 53-76.[2] Mayne et al. (2014) Geosci. Model Dev. 7, 3059–3087.[3] Lenton & Daines (2017) Ann. Rev. Mar. Sci. 9:1, 31-58.[4] Byrne & Goldblatt (2015) Clim. Past 11, 559–570.
Seasonal variation of ozone vertical profiles form ExoMars TGO and comparison to water
Authors: Patel Manish R. , Seller Graham , Mason Jonathon , Holmes James , Brown Megan , Lewis Stephen , Rajendran Kylash , Streeter Paul , Marriner Charlotte , Hathi Brijen , Slade David , Leese Mark , Wolff Mike , Khayat Alain , Smith Michael , Aoki Shohei , Piccialli Arianna , Vandaele Ann Carine , Robert Severine , Daerden Frank ,   the NOMAD Team
Published: July 2021

The Ultraviolet and Visible Spectrometer (UVIS) channel [1] of the Nadir and Occultation for Mars Discovery (NOMAD) instrument [2] aboard the ExoMars Trace Gas Orbiter has been making observations of the vertical, latitudinal and seasonal distributions of ozone.  Here, we present ~1.5 Mars Years (MY) of vertical profiles of ozone, from LS = 163° in MY34 to LS = 320° in MY35.  This period includes the occurrence of the MY34 Global Dust Storm. The relative abundance of both ozone and water (from coincident NOMAD measurements) increases with decreasing altitude below ~40 km at perihelion and at aphelion, localised decreases in ozone abundance exist between 25-35 km coincident with the location of modelled peak water abundances. High latitude (> ± 55°), high altitude (40-55 km) equinoctial ozone enhancements are observed in both hemispheres (LS ~350‑40°).  Morning terminator observations show elevated ozone abundances with respect to evening observations, most likely attributed to diurnal photochemical partitioning along the line of sight between ozone and O. The ozone retrievals presented here provide the most complete global description of Mars ozone vertical distributions to date as a function of season and latitude
NIRPS: the Near-InfraRed Planet Searcher joining HARPS on the 3.6-m
Authors: Grieves Nolan , Bouchy François , Doyon René , Artigau Etienne , Malo Lison , Sosnowska Danuta , Wildi François , Blind Nicolas , Sordet Michael , Segovia Alex
Published: July 2021

The Near-InfraRed Planet Searcher (NIRPS) is designed to be an ultra-stable infrared spectrograph to be installed on ESO’s 3.6 m Telescope in La Silla, Chile. NIRPS is an adaptive optics (AO) fiber-fed spectrograph operating from 0.98 to 1.8 μm and will be operated simultaneously with the optical high-resolution spectrograph HARPS. NIRPS can operate in two modes fed by two different fiber links permanently mounted at the Cassegrain focus that use either 0.4 arcsecond-fibers for the High Accuracy Mode (HAM) or 0.9 arcsecond-fibers for the High Efficiency Mode (HEM). The wavelength range of NIRPS is optimal for low-mass M dwarfs and the simultaneous NIRPS and HARPS observations will improve stellar activity filtering methods given their different wavelength coverages. The NIRPS front-end and AO system were already tested on-sky at La Silla. The spectrograph and back-end is being shipped to La Silla and installed in Summer/Fall 2021. Already we have adapted the state-of-the-art ESPRESSO data reduction pipeline for NIRPS, obtained accurate wavelength solutions with a Uranium Neon lamp, and obtained drift stability results below 50 cm/s with a Fabry–Pérot etalon. We discuss the current and expected instrument performance and the expected results of NIRPS.
Relationship between the ozone and water vapour vertical profiles on Mars observed by NOMAD-TGO
Authors: Piccialli Arianna , Vandaele Ann Carine , Aoki Shohei , Willame Yannick , Depiesse Cedric , Trompet Loic , Neary Lori , Viscardy Sebastien , Daerden Frank , Erwin Justin , Thomas Ian R. , Ristic Bojan , Mason Jon , Patel Manish , Khayat Alain , Wolff Michael , Bellucci Giancarlo , Lopez Moreno Jose Juan
Published: July 2021

IntroductionRecently, [1] characterized the relation between ozone and water vapor using SPICAM simultaneous measurements of O3 and H2O column densities covering four Martian years. They found that O3 and H2O columns are clearly anti-correlated at high latitudes while being uncorrelated at low latitudes.In our study, we take advantage of the NOMAD capability to measure simultaneous vertical profiles of ozone and water vapor to characterize the O3 – H2O relationship at different altitude ranges and latitudes. 1. Ozone and water vapor profile retrievalsNOMAD (Nadir and Occultation for MArs Discovery) is a spectrometer composed of 3 channels: 1) a solar occultation channel (SO) operating in the infrared (2.3-4.3 μm); 2) a second infrared channel LNO (2.3-3.8 μm) capable of doing nadir, as well as solar occultation and limb; and 3) an ultraviolet/visible channel UVIS (200-650 nm) that can work in the three observation modes [2,3].The UVIS channel has a spectral resolution
A New Facility for the Planetary Science Community at DLR: the Planetary Sample Analysis Laboratory (SAL).
Authors: Bonato Enrica , Schwinger Sabrina , Maturilli Alessandro , Helbert Jörn
Published: July 2021

Introduction: Laboratory measurements of extra-terrestrial materials like meteorites and ultimately materials from sample return missions can significantly enhance the scientific return of the global remote sensing data.This motivated the addition of a dedicated Sample Analysis Laboratory (SAL) to complement the work of well established facilities like the Planetary Spectroscopy Laboratory (PSL) and the Astrobiology Laboratories within the Department of Planetary Laboratories at DLR, Berlin. SAL is being developed in preparation to receive samples from sample return missions such as JAXA Hayabusa 2 and MMX missions, the Chinese Chang-E 5 and 6 missions as well as the NASA Osiris-REX mission. SAL will be focusing on spectroscopic, geochemical, mineralogical analyses at microscopic level with the ultimate aim to derive information on the formation and evolution of planetary bodies and surfaces, search for traces of organic materials or even traces of extinct or extant life and presence of water.Sample Analysis Laboratory: The near-term goalis to set up the facilities  on time to receive samples from the Hayabusa 2 mission. The operations have already started in 2018 with the acquisition of a vis-IR-microscope and it will continue with the acquisition of: Field Emission Gun - scanning electron microscope (FEG-SEM), Field Emission Gun – electron microprobe analyser (FEG-EMPA), X-ray diffraction (XRD) system with interchangeable optics for μXRD analysis anda polarised light microscope for high resolution imaging and mappingThe facilities will be hosted in a clean room (ISO 5) equipped with glove boxes and micromanipulators to handle and prepare samples. All samples will be stored under dry nitrogen and can be transported between the instruments  with dedicated shuttles in order to avoid them to enter in contact with the external environment. Based on current planning the first parts of SAL will be operational and ready for certification by end of 2022.Current facilities: To characterize and analyse the returned samples, SAL facilities will work jointly with the existing spectroscopic capabilities of PLL.PLL has the only spectroscopic infrastructure in the world with the capability to measure emissivity of powder materials, in air or in vacuum, from low to very high temperatures [1-3], over an extended spectral range from 0.2 to 200 µm. Emissivity measurements are complemented by reflectance and transmittance measurements produced simultaneously with the same set-up. Recently a vis-IR-microscope was added to extend spectral analysis to the sub-micron scale. In addition, the department is operating a Raman micro-spectrometer with a spot size on the sample in focus of
Azimuthal field signatures associated with magnetosphere-ionosphere coupling in the Jovian magnetosphere: Comparison between Juno observations and theoretical modelling
Authors: Kamran Aneesah , Bunce Emma , Cowley Stanley , Nichols Jonathan , Provan Gabrielle
Published: July 2021

We present a comparison of magnetic field data collected by the NASA Juno spacecraft, with the magnetosphere-ionosphere (MI) coupling model for the Jovian system developed by the University of Leicester. We study the magnetic field of Jupiter, in the Northern Hemisphere, for Perijoves 1-13. By virtue of the offset of the magnetic field to the rotation axis and the subsequent “wobble” of the Juno trajectory in magnetic coordinates, these northern hemisphere portions of PJs 1-13 see the spacecraft traversing the magnetic field lines connecting to the inner, middle, outer and tail regions of the magnetosphere. As such, even away from the close Perijove period, the observations contain evidence of the expected magnetic field perturbations associated with field-aligned currents associated with this fundamental MI coupling. In this study, therefore, we focus on investigating the nature of the field-aligned current signatures evident in the residual azimuthal field (having subtracted the Connerney et al 2018 JRM09 internal magnetic field model) along the magnetic field lines outside of the close periapsides. We map the residual azimuthal field signatures into the ionosphere, and calculate the corresponding ionospheric Pedersen current on an orbit by orbit basis. We compare the magnitude and distribution of these field-aligned current signatures to those expected from the Leicester model, and consider the observed orbit-by-orbit variation as a function of ionospheric colatitude and longitude. We deduce estimates for the field-aligned current densities on auroral field lines for each observation using the Pedersen currents and their distribution in co-latitude, and compare to the previous work of Kotsiaros et al [2019]. We discuss possible reasons for the variations we see, and present the next steps of our broader analysis.
Ganymede Cratering Record
Authors: Martellato Elena , Marchi Simone , Galluzzi Valentina , Palumbo Pasquale , Rotundi Alessandra
Published: July 2021

JUICE, JUpiter ICy moons Explorer, the ESA mission planned to be launched in 2022 and to arrive at Jupiter in 2029, will make detailed observations of Jupiter and three of its largest moons. One of its goals is to improve the current estimates of Ganymede surface age [2].Ganymede was observed firstly by Voyager 1 and 2 in 1979, and then by Galileo between 1996 and 2000 through six flybys, which revealed that the surface has two main types of terrains, which differ in albedo, crater density, and surface morphology [4]. The first one, the “dark” terrains, is low albedo terrains, covered by regolith material, and heavily cratered. The second one, the “light” terrains, has higher albedo and lower crater density, suggesting a younger age. They can occur as smooth elongated and polygonal shaped areas, or as grooves. An accurate chronology for Ganymede can therefore provide information about resurfacing and the evolution of the surface, including the extent of the cryovolcanism [3].As part of the future activities, we make new crater counts to be then used to refine current Ganymede crater-based chronology. The quantitative and statistical analysis of impact crater populations is the primary tool to derive absolute ages of planetary and small body terrains. Further information to improve surface landform interpretation and crater counts can be derived from the crater morphological “freshness”, which may represent a first qualitative hint to the relative ages of individual craters and the surrounding area.The goal of this project is to improve Ganymede crater chronology using the most updated understanding on the current and historical impact flux resulting from recent dynamical models. In this work, we will present our results in i) improving the geological mapping of the Ganymede surface, and in ii) deriving a revised crater database for Ganymede.The present global image mosaic of Ganymede is available at a resolution of ~1 km/pixel. Being only 74% of the surface at a resolution better than 2 km/pixel, either image resampling or degradation was applied [1], [4]. We select the areas of Ganymede acquired at the highest resolution (
Women in Astronomy in Belgium
Authors: Piccialli Arianna , Lefever Karolien , Vandaele Ann Carine , Gielen Clio
Published: July 2021

We are attempting to gather all information available to study the question of the representation of women in astronomy in Belgium, which is not a straightforward task.In an early study, [1] analysed gender-specific statistics on the Belgian physicists. One of the difficulties they found was that Belgium keeps different statistics for the French-speaking and Flemish universities, and the career structure is different depending on the Communities.As preliminary analysis, we investigated the percentage of women in the International Astronomical Union (IAU) registered in the database for Belgium [2]. The IAU is an international organization with participation from 68 countries that covers the main areas of astronomy, including planetary science. In 2021, 32 out of 144 Belgian members were female (22%). It is important to notice that not all astronomers in Belgium, and in particular not the younger generation where the percentage of female researchers is higher, are member of IAU. Therefore we expect these values to underestimate the true number of women in the field. In view of the fact that it is the same at the level of the funding bodies and, by construction, at the universities, Earth and Space Sciences will be considered together. We will present preliminary results of our study.References:[1] Petra Rudolf, Vice‐President, Christine Iserentant, Muriel Vander Donckt, Nathalie Balcaen, Peggy Fredrickx, Karen Janssens, and Griet Janssen, "Women in Physics in Belgium: Still a Long Way From Achieving Gender Equality", AIP Conference Proceedings 628, 131-132 (2002) https://doi.org/10.1063/1.1505297[2] https://www.iau.org/administration/membership/individual/distribution/
Connecting the atmosphere and the interior in extrasolar gas planets
Authors: Schneider Aaron , Carone Ludmila , Decin Leen , Jorgensen Uffe
Published: July 2021

We investigate how radiatively driven heating and cooling in the upper atmosphere (at pressures below 1 bar) influences the interior temperature profile (at pressures between 1 to 700 bar) by means of dynamical heat transport. To achieve this goal, we perform fully coupled 3D-radiation-hydrodymamical models with the new full RT 3D climate model MITgcm/ExoRadPRT for WASP-43 b and HD209458 b. We show in our simulations under which conditions the interior temperature profile converges to a hot deep adiabat. Furthermore, we show if differences occur between the non inflated WASP-43 b and the inflated HD209458 b due to different flow structures at depth for similar irradiation.
Plasma and magnetic field conditions during radar blackouts at Mars.
Authors: Lester Mark , Sanchez-Cano Beatriz , Opgenoorth Hermann
Published: July 2021

Large scale solar wind disturbances such as Interplanetary Coronal Mass Ejections (ICMEs) have a major impact on planetary systems.  At Mars, for example, Solar Energetic Particles released during the process that creates the ICME cause large scale radar blackouts as a result of enhanced ionisation at lower altitudes than normal.  The increased absorption of the radar signals can last for up to 10 – 12 days, depending on the operational frequency of the radar.  These events occur at all latitudes and local times but there does appear to be a peak in occurrence at a solar zenith angle of about 160o, i.e. deep in the tail of the Martian plasma system. Using data from MAVEN, Mars Express and Mars Reconnaissance Orbiter we investigate the background plasma  and magnetic field conditions, which occur at the same time as these events to investigate how the SEP impact on the nightside atmosphere.  This will provide crucial evidence for plasma transport in the Martian system, in particular during the passage of ICMEs.
Mutual radio occultation experiment between ExoMars Trace Gas Orbiter and Mars Express: algorithms testing
Authors: Nava Bruno , Migoya-Orue Yenca , Kashcheyev Anton , Sánchez-Cano Beatriz , Witasse Olivier , Svedhem Håkan , Parrott Jacob , Titov Dimitri , Toni Andrea , Ao Chi
Published: July 2021

Radio Occultation (RO) is a very powerful technique to probe a planetary atmosphere, in providing vertical density profiles of the neutral atmosphere and ionosphere. The standard method uses a radio link between a spacecraft and an Earth ground station. Nevertheless, the possibility to obtain information about the Martian atmosphere with mutual RO events, using data from NASA Mars Odyssey and Mars Reconnaissance Orbiters (MRO), has been demonstrated by Ao et al. (2015).Taking advantage of two European spacecraft in orbit around Mars, the European Space Agency is currently preparing experiments of mutual RO between Mars Express (MEX) and the ExoMars Trace Gas Orbiter (TGO). In preparation of MEX and TGO data inversion and analysis, a simulation-based strategy has been adopted and an algorithm able to retrieve vertical electron density profiles from Doppler shift measurements has been implemented and validated. Subsequently, in order to test the mentioned algorithm with experimental data, the same three RO events considered in the paper by Ao et al. (2015) have been processed. In particular, for each RO event, having the information about the satellites’ orbit, the (excess) Doppler shift values corresponding to the Mars Odyssey-MRO ray-paths have been converted to bending angles as a function of impact parameter. Then, assuming a spherical symmetry (Fjeldbo et al., 1971) for the ionosphere electron density, the bending angles have been transformed (through Abel integral) to a vertical refractivity profile, which, in turn, has been converted to an ionospheric electron density profile.In this work, the results obtained by the application of the mentioned inversion algorithm to experimental data will be presented, with particular focus on the retrieval of the ionospheric electron density profiles.ReferencesAo, C. O., C. D. Edwards Jr., D. S. Kahan, X. Pi, S. W. Asmar, and A. J. Mannucci (2015), A first demonstration of Mars crosslink occultation measurements, Radio Sci., 50, 997–1007, doi:10.1002/2015RS005750.Fjeldbo, G., A. J. Kliore, and V. R. Eshleman (1971), The neutral atmosphere of Venus as studied with the Mariner V radio occultationexperiments, Astron. J., 76, 123–140.
The stellar occultations by the largest satellite of the dwarf planet Haumea, Hi'iaka
Authors: Fernández-Valenzuela Estela , Ortiz Jose Luis , Holler Bryan , Vara-Lubiano Monica , Morales Nicolas , Sicardy Bruno , Vachier Frederic , Desmars Josselin , Braga-Ribas Felipe , Rustamkulov Zafar , de la Vega Alex , Warner Elizabeth , Conti Dennis , Lecacheux Jean , Francini Richard , Langill Phil , Morales Ruben , Jehin Emmanuel , Fraser Wesley C. , Souami Damya ,   Lucky Star and Hi'iaka's occultation Teams
Published: July 2021

Two stellar occultations by the largest satellite of the dwarf planet Haumea, Hi'iaka, were predicted to happen on April, 6th and 16th, 2021. Additional high accuracy astrometric analysis was carried out in order to refine the prediction for April 6th, using several telescopes in the 1.2-m to 2-m range, with the final shadow path crossing North Africa. We successfully detected the first event from TRAPPIST-North telescope at Oukaïmeden Observatory (Morocco). Although it was recorded from only one site, this first detection allowed us to improve the prediction for the second that crossed North America from East to West. We had a good success recording six positive detections and several negative detections that constrain the shape and size of the body. The light curves obtained from the different observatories provide the time at which the star disappears and reappears, which are translated into chords (the projected lines on the sky-plane as observed from each location). Additionally, we carried out a campaign to study Hi'iaka's rotational light-curve, studying the residuals of Haumea's rotational light-curve to a four-order Fourier fit. We obtained the rotational phases at the times of the occultations, which is critical for the analysis of the occultations, given that Hi’iaka is clearly non-spherical. Our preliminary results show that Hi'iaka indeed has a triaxial shape with a larger effective diameter than what has been published so far. The preliminary results and their implications will be discussed in this talk. 
Exoplanets with ELT-METIS I: Estimating the Direct Imaging Exoplanet Yield Around Nearby Stars within 6.5 Parsecs
Authors: Bowens Rory , Meyer Michael , Delacroix Christian , Absil Olivier , van Boekel Roy , Quanz Sascha , Shinde Muskan , Kenworthy Matthew , Carlomagno Brunella , Orban de Xivry Gilles , Cantalloube Faustine , Pathak Prashant
Published: July 2021

Direct imaging is a powerful exoplanet discovery technique that is complimentary to other techniques with great promise in the era of 30-meter class telescopes. Space-based transit surveys have revolutionized our understanding of the frequency of planets at small orbital radii around sun-like stars. The next generation of extremely large ground-based telescopes will have the angular resolution and sensitivity to directly image planets with R < 4 Earth radii around the very nearest stars. Here we predict yields from a direct imaging survey of a volume-limited sample of sun-like stars with the Mid-Infrared ELT Imager and Spectrograph (METIS) instrument, planned for the 39-m European Southern Observatory (ESO) Extremely Large Telescope (ELT) that is expected to be operational towards the end of the decade. Using Kepler occurrence rates, a sample of stars with spectral types A-K within 6.5 pc, and simulated contrast curves based on an advanced model of what is achievable from coronagraphic imaging with adaptive optics, we estimate the expected yield from METIS using Monte Carlo simulations. We find the METIS expected yield of small planets in the N2 band (10.10 - 12.40 μm) is 1.15 planets which is greater than similar observations in the L (3.70 - 3.95 μm) and M (4.70 - 4.90 μm) bands. We also determine a 42% chance of detecting at least one Jovian planet in the background limited regime assuming a 1-hour integration. We calculate the yield per star and estimate optimal observing revisit times to increase the yield. We also analyze this survey if performed in the northern hemisphere and find there are additional targets worth considering. Finally, we present an observing strategy in order to maximize the possible yield for limited telescope time, resulting in 1.52 expected planets in the N2 band.
FORESAIL-1 and ESTCube-2 Cubesat experiments of Coulomb drag propulsion
Authors: Janhunen Pekka , Toivanen Petri , Kivekäs Jarmo , Meskanen Matias , Polkko Jouni
Published: July 2021

Coulomb drag propulsion taps momentum from a natural plasma stream to generate propellantless low-thrust propulsion for a spacecraft. The plasma is attached to by means of a long, thin, charged metallic tether. The tether's electrostatic field deflects the motion of streaming plasma ions and transfers momentum from them. The technique can be applied in the solar wind (i.e., outside Earth's magnetosphere) to produce general-purpose interplanetar propulsion. This application is called the electric solar wind sail (E-sail). It can also be applied in low Earth orbit (LEO) to brake the satellite's orbital motion. Here the relevant plasma stream is the ram flow of the ionosphere due to the satellite's orbital motion. This application is called the plasma brake and it is useful for satellite deorbiting for mitigating the growing problem of orbital debris.Here we report on progress of two CubeSat missions (FORESAIL-1 and ESTCube-2) that are under construction for measuring the Coulomb drag effect in LEO.  Both are scheduled to fly in 2022. Both satellites deploy up to 300 m long tether, charge it up by a high-voltage source and measure the resulting Coulomb drag. The satellites are slowly spinning and the tether is tightened by the centrifugal force. The tether is deployed from a reel which is rotated slowly by an electric motor.  Both satellites use negative tether polarity, which is the case relevant for the plasma brake. ESTCube-2 contains, in addition, a positive mode experiment which is relevant for the E-sail. The plasma environment in LEO differs from the solar wind, so the measured positive mode Coulomb drag must be scaled to yield a prediction of the strength of the E-sail effect in the solar wind.The Coulomb drag is measured by two independent methods. In the first method we set the tether voltage on and off in sync with the satellite's rotation and thereby accumulate a change of the system's angular momentum. The Coulomb drag is inferred from the measured change of the spin rate per time unit. In the second method we estimate Coulomb drag from the speeded-up lowering of the satelllite's orbital altitude.The presentation is a status report of the technical progress of these two Coulomb drag CubeSat missions; FORESAIL-1 and ESTCube-2.
Promoting gendered structural change in leadership in higher education
Authors: Vilhena Fernanda Campanini , Pérez Jon Pizarro
Published: July 2021

Introduction and objectives. In the higher education and research sector, efforts have been employed in diverse countries to bring about gendered structural change, and most strategies pursue such a goal through the implementation of formal changes in its structures and policies. Leaning on the feminist institutionalism theory, the aim of this article is to discuss the importance of understanding how the formal and the informal institutional norms interact between each other in initiatives seeking gender equality in leadership and decision-making in the specific context of higher education institutions. Methodology. A qualitative approach has been followed. Interviews with members of the Board of Directors of a higher education and research institution in northern Spain have been conducted and analysed, aiming at identifying the barriers to the access of women to leadership positions and possible measures to overcome them. Results. The analysis confirmed the impact caused by the gendered dynamics present at both individual and institutional levels to GE initiatives. While the importance of formal institutional commitments to gender equality has been recognised, the analysis recalls the attention to the fact that informal settings shape the applicability of formal policies, with continuous references to the traditionally unequal distribution of power and attribution of value to women and men. Discussion and added value. Although much theoretical knowledge has been produced in the field of gender and institutions, especially concerning the gendered bases of institutions, the field still lacks within-process studies on the aspects influencing the obtained outcomes of developed initiatives pursuing gender equality in institutional leadership. The study developed in this paper allows for replication in different contexts, hence contributing to the refinement of the existing knowledge on the dynamics of change in gender-oriented initiatives
BOLEHKAH ORANG KRISTEN DI KOTA WISATA BATU BERCERAI?
Authors: Efruan Erni M.C.
Published: July 2021

Pada saat kini tingkat perceraian di Indonesia sangat memprihatinkan. Sebuah surat kabar harian dengan berani mengusung tema “Perceraian Darurat Di Indonesia!” Badan Kependudukan dan Keluarga Berencana Nasional (BKKBN) memperingatkan bahwa angka perceraian di Indonesia adalah yang tertinggi di Asia Pasifik. Di antara jumlah permohonan perceraian yang masuk tahun 2019 tercatat 604.997 kasus, 79 persen permohonan telah dikabulkan pengadilan. Lebih dari 479.618 pasangan menikah telah resmi bercerai. Mengejutkannya, perkara kasus perceraian yang diajukan dari pihak istri (Cerai Gugat) totalnya mencapai 355.842 kasus. Artinya penggugat cerai oleh istri sebanyak 70 persen. Sedangkan kasus perceraian yang diajukan dari pihak suami (Cerai Talak) mencapai 124.776 kasus. Di Jawa Timur, Januari hingga Mei 2016 terdapat 3.063 pengajuan kasus perceraian. Total 2.032 istri yang menuntut perceraian terhadap suaminya. Data pada Kemenag Kota Batu tercatat 300 kasus perceraian dan 300 pernikahan dini terjadi dari 1.678 perkawinan pada tahun 2018. Dengan demikian latar belakang penelitian adalah: Apakah orang Kristen di Kota Wisata Batu, Jawa Timur juga berkontribusi pada peningkatan angka perceraian di Indonesia? Bolehkah orang Kristen bercerai? Bagaimana tanggapan Yesus Kristus menurut Injil Markus 10: 1-12? Tujuan penelitian adalah menemukan jawaban Yesus dalam Injil Markus 10: 1-12 sebagai perspektif yang dapat ditimplementasikan dan antisipatif terhadap meningkatnya jumlah kasus perceraian di Kota Wisata Batu, Jawa Timur. Pendekatan terhadap topik “Bolehkah Orang Kristen Di Kota Wisata Batu, Jawa Timur Bercerai?” menggunakan Metode Deskripsi. Hasil analisis literatur menyimpulkan bahwa Yesus Kristus tidak pernah mengizinkan perceraian pasangan Kristen dengan alasan apa pun. Tidak pernah! Hasil survei lapangan menunjukkan bahwa ada kasus perceraian, tetapi tidak terdaftar di Kantor Pemerintah terkait di Kota Wisata Batu, Jawa Timur. Oleh karena itu, penyelidikan ini masih terbuka untuk penelitian lebih lanjut, mengapa ada dua kasus perceraian pada pasangan Kristen di Kota Wisata  Batu, Jawa Timur, namun tidak terdaftar di Instansi Pemerintah?
UPAYA GEREJA DALAM PEMBINAAN USIA REMAJA YANG MELAKUKAN HUBUNGAN “FREE SEKS”
Authors: Illu Wilianus , Masihoru Olivia
Published: July 2021

Free Sex dan hamil pranikah menjadi potret buram kehidupan remaja saat ini di Indonesia. Seks bebas (free sex), hamil di luar nikah, aborsi, perkosaan, pelecehan seksual,  peredaran VCD porno, pornografi, dan pornoaksi merajalela di kalangan remaja saat ini. Hal ini pada satu sisi dapat merisaukan public pada umumnya, misalnya merisaukan lingkungan masyarakat, dunia pendidikan keluarga, sekolah bahkan pendidikan di gereja. Akan tetapi pada aspek lain terdapat orang-orang yang memiliki dorongan yang berangkat dari hati nuraninya sehingga memiliki kepedulian dan keberpihakan terhadap para remaja yang melakukan hubungan free sex. Tipikal yang demikian memiliki inisiatif sendiri untuk menolong orang-orang yang mengalami dan khususnya bagi remaja. Biasanya perihal yang dilakukan adalah berinisiasi untuk mengumpulkan mereka dan menyampaikan materi-materi yang berkaitan dengan free sex agar mengurangi lajunya pergerakan yang semakin dinamis dalam realiata yang ada.

         Pada umumnya Etika Kristen tidak membenarkan tentang hubungan seks bebas atau free sex, baik yang dilakukan oleh oknum-oknum yang berkeluarga, orang dewasa dalam hal ini yang belum menikah, ataupun oleh pemuda-pemudi bahkan remaja-remaja. Upaya Kristen dalam menangani kasus-kasus yang terjadi pada remaja tentu mengacu pada beberapa pola yang sesuai standar Alkitab. Pola-pola yang penulis maksudkan adalah upaya melalui tinjauan Alkitab tentang seksualitas, melalui pendidikan gereja, melalui pendidikan  keluarga, sekolah, melalui pendekatan kontribusi terhadap budaya, masyarakat, dan melalui kontribusi terhadap pemerintah setempat. Supaya elemen-elemen tersebut saling interdepedensi dalam mengatasi free sex yang belakangan ini marak terjadi di kalangan para remaja di Indonesia. Metode yang digunakan dalam kajian jurnal ini adalah metode deskiptif dengan pendekatan literatur dan fakta data sesuai yang berkorelasi dengan judul utama dan sub-sub judul.  Hasil yang ditemukan dalam kajian ini mencakup peran gereja tidak terbatas pada internal gereja melainkan berperan akif  juga di luar gereja khususnya peran dalam mengantisipasi lajunya free sex yang signifikan.
SATISFACTION OF OUTPATIENTS IN WARD OF CONSULTING ROOM, TIEU CAN GENERAL HOSPITAL, IN TRA VINH PROVINCE IN 2020
Authors: Võ Tứ Cường , Lưu Quốc Toản , Đặng Văn Giang , Trần Quốc Thắng , Phạm Ngọc Châu
Published: July 2021

Research on the satisfaction of 260 outpatient patients at Tieu Can general hospital. Methodology: Cross-sectional studies. Interview the subjects with the hospital quality assessment toolkit of the MOH. Results: The results show that, an accessibility satisfaction was 41.9%. Transparency of information and medical examination and treatment procedures reached 47.7%, facilities and equipments for patients reached 58.1%. Satisfaction, behavioral attitude, professional capacity of health workers reached the rate of 33.1%, satisfaction with the quality results of service delivery 37.3%. Conclusion: Patient satisfaction on outpatient care is relatively low.
THE CURRENT SITUATION OF HUMAN RESOURCE AND SOME INFLUENCING FACTORS AT SONG CAU DISTRICT HEALTH CENTER IN 2017-2019
Authors: Nguyễn Thị Tường Lịnh , Phan Văn Trọng , Phùng Thanh Hùng
Published: July 2021

The cross-sectional description research, combining quantitative and qualitative aims to fulfill two objectives: (1) To describe the current situation of human resource and (2) To analyze factors affecting the current situation of human resource at Song Cau District Health Center in 2017-2019. The research results show that the quantity of preventive healthcare personnel complies with the current regulations, and the workfore has an appropriate age (53.9% is 30 - 50 years old). Regarding structure of expertise, it is still inappropriate with low proportion of doctor (10.4%). In term of educational level, the proportion of undergraduate health worker (including doctor) at the Health Center (71.4%) is higher than the overall national proportion, while this proportion at Health Station is lower (8.8%). Some of the factors positively influence the current situation of human resource including: benefit policies under Resolution 110/2014/NQ-HDND; improved human resource planning and recruitment process; the infrastructure system; improved employee evaluation process; encouragement for training. Besides, some negative influencing factors include: unclear employee evaluation; lack of funding to support training; low income.
HEALTH HUMAN RESOURCES AND MEDICAL EXAMINATION ACTIVITIES OF CENTRAL ENDOCRINE HOSPITAL, 2015-2020
Authors: Bùi Minh Thu , Đào Văn Dũng , Bùi Thế Nghĩa
Published: July 2021

Objectives: To describe the current situation of health human resources and medical examination and treatment activities of the Central Endocrine Hospital 2015-2020. Research methodology: Cross-sectional descriptive study combining quantitative research methods (secondary data) and qualitative research (in-depth interviews) with 21 employees working at the Central Endocrine Hospital Results: The ratio of medical staff / hospital beds of the hospital is currently 0.95 lacking compared to the regulations # 08; Administrative and managents staff at the time of the study accounted for 23.24% higher than the prescribed rate; The ratio of doctors / other professional titles (nurses, technicians) is 1 / 2.2, lower than the regulation; The ratio of university pharmacists / doctor is 1/10, meeting the standards; The ratio of university pharmacists / secondary pharmacists is 1 / 1.7, lower than prescribed; The rate of female staff is 65.0% higher than that of men, 35%. The number of medical services, inpatient treatments and surgery all tend to increase from 2015 to 2019. Conclusion: The people’s need for medical examination and treatment is increasing, leading to the increasing workload, the hospital is overloaded. Hospitals need to develop a plan to supplement human resources to suit the scale and structure to better serve the health care activities of the people.
APPROACH TO DISEASE MANAGEMENT CONCEPTS AND CONTENT
Authors: Đào Văn Dũng , Trần Quốc Thắng
Published: July 2021

Disease management is a holistic approach to care for patients in the residential community, integrating holistically and continuously to minimize preventable events by maximizing compliance of patients with health care and promotion behaviors according to regulations. These programs produce significant improvements in health, as well as financial savings. This article initially approaches the concept and main content of disease management and chronic disease management programs.
AVASCULAR NECROSIS OF FEMORAL HEAD: CLINICAL FEATURE, XRAY AND MRI IMAGING, AND RISK FACTORS
Authors: Phan Bá Hải , Ngô Văn Toàn
Published: July 2021

Objective: Describing clinical feature, Xray and MRI imaging, and risk factors on avascular necrossis (AVN) of femoral head Patients and method: studied prospectively 120 AVN patients were diagnosed and operated at Vieduc University Hospital Results: Averave age 47,7 ± 10. Male: Female 11:1. Bilateral AVN of the hip patients are 83,33%. Average time between bilateral AVN of the hip is 6,5 months. Risk factors are alcohol (87,5%) and smoking abuse (58,3%). Xray imaging group normaly in lately stage: cresent sign, collapsed. MRI can detech AVN in early stage (I, II) 44,27% patients Conclusion: AVN is a progressive disease, especially in younger patient. Risk factors is alcohol and smoking abuse. Xray and MRI imaging are valuable for avascular necrossis of femoral head diagnosis