bluuebunny/crossref_metadata_2025 huggingface dataset:
Exoplanet Ephemeris Maintenance using Ground- and Space-based Telescopes
Authors: Caines Hamish , Rocchetto Marco , Savini Giorgio
Published: October 2020

Ariel will require precise knowledge of the transit timings for all of its targets. However, the precision we have for each target will degrade significantly over the 8 years until launch, in some cases to the point where the error exceeds the duration of the transit itself. The knowledge of these transits would then be deemed “lost”. To counteract this, and in effect “reset the clock”, we aim to use the Telescope Live network of robotic telescopes to observe such targets. With 1000 targets and an average orbital period of the order of days, the size and usage of the network required needs to be quantified. Here we present results from simulations of these observations for a variety of telescope networks of varying sizes, the number of targets that can be successfully constrained, and the amount of observing time required to do so. From these results we can conclude that a ground-based telescope network containing as few as 2 telescopes of 0.6m aperture can constrain over 60% of the targets with transit depths observable from the ground. A fraction of these exoplanets are difficult to observe with ground-based telescopes as they either have transit depths too shallow to detect due to atmospheric distortion and/or their transit durations are comparable to the length of a night, reducing the probability of observable transits occurring. Such targets would benefit from supplementary observations from space-based observatories, as these do not suffer from either atmospheric distortion or limits on observing time due to Earth’s diurnal cycle.
Possible effects of Mercury surface temperatures on the exosphere
Authors: Rognini Edoardo , Mura Alessandro , Capria Maria Teresa , Zinzi Angelo , Milillo Anna , Galluzzi Valentina
Published: October 2020

The BepiColombo mission is the first European mission to Mercury; the spacecraft will reach its destination in December 2025, and will study in detail the surface, the exosphere and the magnetosphere of the planet. 

We have developed a thermophysical model with the aim to analyze the dependence of the temperature of the surface and of the layers close to it on the assumptions on the thermophysical properties of the soil. The code solves the one-dimensional heat equation, assumes purely conductive heat propagation and no internal heat sources; the surface is assumed to be composed of a regolith layer with high porosity and density increasing with depth. The illumination conditions are calculated by using a Mercury shape model and the SPICE routines [1]. 

The model will help us to interpret the data that will be provided by the instruments onboard the BepiColombo mission. Preliminary calculations have been carried out to analyze the thermal response of the soil as a function of thermal conductivity. The model is currently also used to study the sodium content in the planet's exosphere, whose origin is under investigation [2]; the MESSENGER mission has measured the exospheric sodium content as a function of time, detecting an increase at the "cold poles" (so called because of their lower than average temperature). We therefore want to study the effect of surface temperatures on the sodium content in the exosphere; for this purpose, the temperature distribution calculated with the code is used together with an atmospheric circulation model that calculates the exospheric sodium content [3]. 

A simplified version of the thermophysical code is almost ready to be available to the scientific community through MATISSE [4], the software developed at the SSDC in ASI and available at https://tools.ssdc.asi.it/Matisse. 
[1] Acton, C. H. (1996), Planetary and Space Science, 44, 65-70[2] Cassidy, T., et al. (2016), GRL, 43, 11 121-128[3] Mura, A., et al. (2009), Icarus, 1, 1-11[4] Zinzi, A., et al. (2016), Astronomy & Computing, 15, 16-28
Simulating Variability due to Faculae and Spots on GKM Stars
Authors: Johnson Luke , Unruh Yvonne , Norris Charlotte , Solanki Sami , Krivova Natalie , Witzke Veronika , Shapiro Alexander
Published: October 2020

Stellar variability is a dominant noise source in exoplanet surveys and results largely from the presence of photospheric faculae and spots. The implementation of faculae in lightcurve models is an open problem, with scaling based on spectra equivalent to hot stellar atmospheres or assuming a solar-derived facular contrast. We model the lightcurves of active late-type stars as they rotate, using emergent intensity spectra calculated from 3D magnetoconvection simulations of G, K and M-type stellar atmosphere regions at different viewing angles to reproduce centre-to-limb brightness variations. We present mean expected variability levels for several cases and compare with solar and stellar observations. We also investigate the wavelength dependence of variability. Fig. 1: Example of our geometrically accurate lightcurve modelling approach. Top: normalised intensity maps of a limb darkened, solar-type star viewed in the \textit{Kepler} band at rotational phase 0.5 with stellar inclinations 90 deg (left) and 30 deg (right). At 90 deg, the star is viewed equator-on. Middle: Corresponding lightcurves calculated at inclinations 90 deg (black line) and 30 deg (red line). Bottom: HealPix map representing the active stellar surface, cosine-scaled in latitude and flattened in longitude to resemble a solar synoptic map. The quiet photosphere is displayed in orange, facular regions are bright yellow and spot regions are dark blue. The crosses represent the centres of the stellar discs in the top panel. Fig. 2: Example showing simulated lightcurves calculated at different wavelengths. Rotational lightcurves are on the left, transit lightcurves on the right. In the centre, one hemisphere of the simulated stellar surface is shown, with a quarter of the disc shown in each wavelength band. 'Giant' spots and facular regions are used in this example. The transit path is highlighted in grey.
Titan’s neutral atmosphere seasonal variations up to the end of the Cassini mission
Authors: Coustenis Athena , Jennings Donald , Achterberg Richard , Lavvas Panayotis , Bampasidis Georgios , Nixon Conor , Flasar F. Michael
Published: October 2020

In our recent publication [1] we reported new results concerning the seasonal atmospheric evolution near Titan’s poles and equator in terms of temperature and composition using nadir spectra acquired by the Cassini Composite Infrared Spectrometer (CIRS) at high spectral resolution during the last year of the Cassini mission in 2017 complementing previous investigations covering almost two Titan seasons. In previous papers [2,3], we reported on monitoring of Titan’s stratosphere near the poles after the mid-2009 northern spring equinox. In particular we have reported on the observed strong temperature decrease and compositional enhancement above Titan’s southern polar latitudes since 2012 and until 2014 of several trace species, such as complex hydrocarbons and nitriles, which were previously observed only at high northern latitudes. This effect accompanied the transition of Titan’s seasons from northern winter in 2002 to northern summer in 2017, while at that latter time, the southern hemisphere was entering winter. Our new data, acquired in 2017 and analyzed here, are important because they are the only ones recorded since 2014 close to the south pole in the mid-infrared nadir mode at high resolution. A large temperature increase in the southern polar stratosphere (by 10-50 K in the 0.1 to 0.01 mbar pressure range) is found associated with a change in the temperature profile’s shape. The 2017 observations also show a related significant decrease in most of the southern abundances which must have started sometime between 2014 and 2017 [1]. For the north, the spectra indicate a continuation of the decrease of the abundances which we first reported to have started in 2015 and small temperature variations [1]. We discuss comparisons with other results and with current photochemical and dynamical models which could be updated and improved by the new constraints set by the findings presented here.[1] Coustenis et al., 2019, Icarus 344, 1 July 2020, 113413 ; [2] Coustenis et al., 2016, Icarus 270, 409-420; [3] Coustenis et al., 2018, Astroph. J. Lett. 854, no2.
Particle Motions in Planetary Magnetic Fields: Europlanet Service
Authors: Guio Patrick , Achilleos Nicholas , André Nicolas
Published: October 2020

The trapping of charged particles in planetary magnetic fields is a process which underpins many important aspects of planetary magnetospheres, such as ring current evolution, particle acceleration, and the flow of current through the system, both free and bound. As part of our effort for the Europlanet project, the UCL group have developed codes which accurately model the trajectories of charged particles in magnetic field models appropriate for the magnetospheres of Jupiter and Saturn. These will form the basis of a service for the SPIDER task. In this presentation, we show examples of ion trajectories at both planets for representative 'start values' of equatorial distance, pitch angle, and values of particle energy. The simulations provide an indication of how particle orbits become less adiabatic as one approaches energies where gyroradii become comparable to magnetic field curvature radius. The disk-like fields of the gas giants are particularly effective at 'scattering' adequately high-energy particle trajectories as they cross the equator, where the field lines are most 'pinched' and have the smallest length scales.
Temperature, chemical species and wind distributions in the middle atmosphere of Titan from late northern spring to early summer
Authors: Vinatier Sandrine , Mathé Christophe , Bézard Bruno , Vatant d'Ollone Jan , Lebonnois Sébastien , Dauphin Cyril , Flasar F. Mike , Achterberg Rich K. , Seignovert Benoît , Sylvestre Melody , Teanby Nick , Gorius Nicolas , Mamoutkine Andrei , Guandique Ever , Jennings Don
Published: October 2020

We present a study of the seasonal evolution of Titan’s thermal field and distributions of haze, C2H2, C2H4, C2H6, CH3C2H, C3H8, C4H2, C6H6, HCN and HC3N from March 2015 (Ls = 66°) to September 2017 (Ls = 93°), i.e. from the last third of northern spring to early summer. We analyzed thermal emission of Titan’s atmosphere acquired by the Cassini Composite Infrared Spectrometer (CIRS) with limb and nadir geometry to retrieve the stratospheric and mesospheric temperature and mixing ratios pole-to-pole meridional cross sections from 5 mbar to 50 μbar (120-650 km).The southern stratopause varied in a complex way and showed a global temperature increase from 2015 to 2017 at high-southern latitudes. Stratospheric southern polar temperatures, which were observed to be as small as 120 K in early 2015 due to the polar night, showed a 30-K increase (at 0.5 mbar) from March 2015 to May 2017 due to adiabatic heating in the subsiding branch of the global overturning circulation. All photochemical compounds were enriched at the South Pole by this subsidence. Polar cross sections of these enhanced species, which are good tracers of the global dynamics, highlighted changes in the structure of the southern polar vortex. These high enhancements combined with the unusually low temperatures (
Nebular condensation of different stellar compositions and its influence on planetary chemistry
Authors: Wang Haiyang , Sossi Paolo , Quanz Sascha
Published: October 2020

The volatility of an element is defined by its 50% condensation temperature (Tc50) from a canonical nebular gas of Solar composition at 10-4 bar [1, 2]. However, the variability in metallicity and metal/oxygen ratios of extrasolar systems inferred from the spectroscopic measurements of their parent stars [3, 4] implies that the identity, abundance and sequence of condensation may deviate from that of our solar system. As such, planets formed at similar heliocentric distances may be expected to have distinct compositions from those of the terrestrial planets in our solar system. Here we investigate the degree to which nebular composition influences the condensation process by taking nine sets of stellar compositions with variable metallicities that span the range from -0.4 to +0.4 dex and performing Gibbs free energy minimisation calculations with FactSage, including treatment of mineral solid-solutions,  over the temperature range 1723 K to 473 K.  We find that, although the general order of condensation is similar, absolute values of Tc50 are shifted to higher temperatures at higher dex, where Tc50(S), in particular, increases relative to those of other elements. Condensing nebulae with high metallicities (and also high metal/oxygen ratios) also exhibit the following features: (i) the appearance of reduced assemblages (e.g. CaS oldhamite, forsterite-rich olivine and graphite) in the condensates, (ii) increased fractions of oxygen (relative to its total abundance) locked in the silicate condensates, and (iii) lower fO2 in the gas phase. As a result, these characteristics will lead to significant differences in the chemistry of planetary building blocks, which are then accreted to form telluric planetary bodies. References[1] Lodders 2003. ApJ 591:1220-1247. [2] Wood, B. J., Smythe, D. J., & Harrison, T. 2019. Ame. Miner. 104:844-856.[3] Buder, S., Asplund, M., Duong, L. et al. 2018. MNRAS 478:4513:4552.[4] Delgado Mena, E., Moya, A., Adibekyan, V., et al. 2019. A&A 624:A78.
Chromites in Ordinary chondrite fusion crusts
Authors: Bellesi Manlio , Manzetti Francesco , Pratesi Giovanni , Giuli Gabriele
Published: October 2020

We studied 5 fall Ordinary Chondrites of different groups (H4, H5, LL5, LL6, L3.6) and an Antarctic meteorite (H5), in order to investigate possible compositional differences between the chromites present in the bulk and the chromites formed within the fusion crust. We report here the composition of about 50 chromites measured within the bulk and 70 chromites found in the crust.Chromites found in the bulk are usually anhedral and relatively large in size (several tens of micrometers), whereas chromites formed within the crust are consistently smaller (few micrometers in size) and can display anhedral, or subhedral to euhedral habit.The Mg# and Al# determined for all the chromites found in the bulk show a fair agreement with data reported in the literature for chromite compositions in ordinary chondrites (Bunch et al., 1967; Ramdohr, 1967; Rubin, 2003; Wlotzka, 2005), which display a small scatter of the Al# (ca.0.13±0.025) and a large variation of the Mg# (from 0.05 to 0.30).When compared with the ones found in the bulk, chromites found within the fusion crusts generally exhibit similar values of the Al#; however, they display a much larger scatter of the Mg# and, usually, also larger average Mg# (up to 0.65) than their conterparts in the bulk.Chromite in the fusion crusts are often associated to magnetite dendrites made up by magnetite octahedral crystals 200-400 nanometers wide; occasionally, other spinel group minerals can be found, as magnesiochromites and magnesioferrites. In most of the samples studied, several chromite crystals are mantled by magnetite crystals, whereas no magnetite crystal has been found mantled by chromites. Textural data so far collected suggest a crystallization sequence in the fusion crust: Olivine, Chromite, Magnetite. References:Bunch T.E., Keil K. and Snetsinger K.G. (1967). Chromite composition in relation to chemistry and texture of ordinary chondrites. Geochimica et Cosmochimica Acta, 31, 1569-1582.Ramdohr P. (1967). Chromite and chromite chondrules in meteorites-I. Geochimica et Cosmochimica Acta, 31, 1961-1967.Rubin A.E. (2003). Chromite-Plagioclase assemblages as a new shock indicator; implications for the shock and thermal histories of ordinary chondrites. Geochimica et Cosmochimica Acta, 67, 2695–2709.Wlotzka F. (2005) Cr spinel and chromite as petrogenetic indicators in ordinary chondrites: Equilibration temperatures of petrologic types 3.7 to 6. Meteoritics and Planetary Science, 40, 1673-1702 
The Hilbert-Huang Transform (HHT) as a tool for characterizing dynamical features of Mercury’s and Venus’ magnetospheres
Authors: Alberti Tommaso , Milillo Anna , Laurenza Monica , Massetti Stefano , Ivanovski Stavro , Ippolito Alessandro , Plainaki Christina , De Angelis Elisabetta , Mangano Valeria , Mura Alessandro , Orsini Stefano , Rispoli Rosanna
Published: October 2020

The interaction between the interplanetary medium and planetary environments gives rise to different phenomena according to the spatio-temporal scales. Here we apply for the first time a novel data analysis method, i.e., the Hilbert-Huang Transform, to discriminate both local and global properties of Venus’ and Mercury’s environments as seen during two MESSENGER flybys. Hence, we may infer that the near-Venus environment is similar in terms of local and global features to the ambient solar wind, possibly related to the induced nature of Venus’ magnetosphere. Conversely, the near-Mercury environment presents some different local features with respect to the ambient solar wind, due to both interaction processes and intrinsic structures of the Hermean environment. Our findings support the ion kinetic nature of the Hermean plasma structures, with the foreshock and the magnetosheath regions being characterized by inhomogeneous ion-kinetic intermittent fluctuations, together with MHD and large-scale fluctuations, the latter being representative of the main structure of the magnetosphere. We also show that the HHT analysis allow to capture and reproduce some interesting features of the Hermean environment as flux transfer events, Kelvin-Helmholtz vortex, and ULF wave activity, thus providing a suitable method for characterizing physical processes of different nature. Our approach demonstrate to be very promising for the characterization of the structure and dynamics of planetary magnetic field at different scales, for the identification of different planetary regions, and for the detection of the “effective” planetary magnetic field that can be used for modelling purposes.
The art of exploring
Authors: De Toffoli Barbara , Pozzobon Riccardo , Montagna Carlotta , Schiavo Jacopo , Scotton Bianca Maria , Fantino Ivan , Massironi Matteo
Published: October 2020

Within the European Horizon-2020 project PlanMap - whose aim is to provide integrated cartography with spectral information, stratigraphy and 3D geologic models of the subsurface - several artists contributed in shaping the vision of geological exploration of planetary bodies of our Solar System for the wide public (https://planmap.eu/content/artists). We addressed a broad audience of kids, students and general public by means of dedicated artworks and the production of a project soundtrack. We realised the following initiatives: (a) The “Drawing for Kids” storyline tells the adventures of the project's mascot Geolyn who is portrayed in stand-alone contexts related to planetary geology and exploration. These paintings aim to present geological mapping to the young public depicting in a very friendly and simple way the mapping process; (b) The “Drawing the Future” illustrations aim to deliver the vision of a near future where the tools and the scientific products of Planmap become hands-on applications for the exploration of the Moon, Mars and Mercury. This storyline aims to engage secondary school students and the general public showing planetary landscapes explored through enhanced tools and augmented reality; (c) “Drawing the Comic” is an initiative that is regularly published in the PLaNCK! Magazine (www.planck- magazine.it) and narrates the adventures of Marie, Max, Planck and nanny Rose delivering accurate and correct scientific information using vocabulary and narrative strategy suitable for the target audience; (d) The Planmap soundtrack project led to the realization of a dedicated multi-instrument track within the ITH project which aims to explore the baffling emotions and feelings of dreams from the point of view of a blind child. ITH is a one man band project with exploration desire at its core and each song has references to space, stars and science. This initiative is supported by the European Union’s Horizon 2020 research and innovation program under grant agreement N°776276 (PLANMAP).
Channelling Our Efforts: Europlanet in Social Media
Authors: Usher Helen , Roberts Sarah , Heward Anita
Published: October 2020

The (small) Europlanet social media team has agreed aims of: Informing, Enthusing, Engaging, Encouraging and Celebrating the European Planetary Science Community and the wider community too.  Their work supplements the more traditional channels of website, newletters and mailing lists. But how can this be done most effectively?  What channels should be used?  What content? What frequency? If the needs of the communities are to be met, they first need to be identified.  There is currently a lack of data for this. The proposed interactive poster will pose some questions for the community to consider during EPSC2020, link to a survey for data collection, and use the interactive, virtual nature of the meeting to stimulate a wide discussion.  The data and views of the community will then be used to inform the social media communication strategy for the remainder of the Europlanet 2024 RI Programme.
Heavy ion charge states in Jupiter’s polar magnetosphere inferred from auroral megavolt electric potentials
Authors: Clark George , Mauk Barry , Kollmann Peter , Paranicas Chris , Bagenal Fran , Allen Robert , Bingham Sam , Bolton Scott , Cohen Ian , Ebert Robert , Dunn William , Haggerty Dennis , Houston Steve , Jackman Caitriona , Roussos Elias , Rymer Abi
Published: October 2020

In this presentation, we exploit the charge-dependent nature of field-aligned potentials in Jupiter’s polar cap auroral region to infer the charge states of energetic oxygen and sulfur. To-date, there are very limited and sparse measurements of the > 50 keV oxygen and sulfur charge states, yet many studies have demonstrated their importance in understanding the details of various physical processes, such as, X-ray aurora, ion-neutral interactions in Jupiter’s neutral cloud and particle acceleration theories. In this contribution, we develop a technique to determine the most abundant charge states associated with heavy ions in Jupiter’s polar magnetosphere. We find that O+ and S++ are the most abundant and therefore iogenic in origin. The results are important because they provide 1) strong evidence that soft X-ray sources are likely due to charge stripping of magnetospheric ions and; 2) a more complete spatial map of the oxygen and sulfur charge states, which is important for understanding how the charge- and mass-dependent physical processes sculpt the energetic particles throughout the Jovian magnetosphere. 
Spectral and morpho-stratigraphic units integration on Apollo basin and Leibnitz/Von Karman craters on the Moon
Authors: Zambon Francesca , Carli Cristian , Altieri Francesca , Combe Jean-Philippe , van der Bogert Carolyn H. , Pöler Claudia , Hiesinger Harald , Le Mouélic Stephane , Mangold Nicolas , Caravaca Gwénaël , Massironi Matteo
Published: October 2020

South Polar Aitken (SPA) is the largest and deepest basin on the Moon [1, 2], and several regions within this widespread basin have been considered as possible landing sites for present and future missions. Some of these sites are also targets of the H2020 n° 776276- PLANMAP project [3]. In this work, we focus on specific areas within SPA, Apollo basin, Lebinitz and Von Karman craters regions (see fig. 1). For our analysis, we considered the M3/Chandrayaan-1 data [4], after the application of the last calibration, thermal removal and photometric correction [5, 6].SPA is rich in high Ca-pyroxenes, except for some central crater peaks, where low Ca-pyroxenes dominate, and no extensive olivine-rich areas are observed [1, 7, 8]. Based on the spectral characteristics on the M3 spectra, we define specific spectral parameters, such as band centers, depths, spectral slopes, including selected RGB color composite combinations [5]. These indices are the starting point for retrieving the spectral units of the regions considered. The final aim of this work is to find a link between spectral, and morpho-stratigraphic units [9] to reach out highly informative geological maps of the Moon. This innovative approach holds the efforts of different research units and is one of the main goals of the PLANMAP project. References: [1] Ohtake, M. et al., 2014, GRL. [2] Moriarty, D.P. et al., 2018, JGR. [3] https://www.planmap.eu/, [4] Pieters et al., 2009, Current Science., [5] PLANMAP D4.3- Spectral Indices and RGB maps. [6] Besse, S. et al., 2012, Icarus. [7] Dhingra, D., 2018, Geosciences. [8] Melosh, H. J., et al., 2017, Geology. [9] Ivanov, M.A., 2018, JGR. Acknowledgments: This work is funded by the European Union’s Horizon 2020 research grant agreement No 776276- PLANMAP.  Figure 1: Apollo basin (top-left) and Leibnitz and Von Karman craters (bottom-left) reflectance map at 540 nm. Apollo basin (top-right) and Leibnitz and Von Karman craters (bottom-right) Clementine-like mosaic derived by M3 data (bottom-right).
The effect of late gas disks on the late stages of planet formation
Authors: Kral Quentin
Published: October 2020

The external supply of gas to planetary atmospheres may be important to set their final compositions. In this talk, I will summarize recent works that quantified in an exoplanetary context, how much gas can be delivered to planets from late gas disks, which appear to be rather ubiquitous around main-sequence stars with bright planetesimal belts. This new gas component is indeed found to be present for tens and sometimes hundreds of millions of years around main-sequence stars. The gas is thought to be released from planetesimals when they collide together in their parent belt, which creates a gas disk (made of volatiles) that can viscously spread further in the system and encounter the already formed planets that can capture this gas, which will affect the primordial atmospheres of these planets. Kral et al. (2020) show that this very late accretion onto planets is very efficient and may allow capturing large quantities of carbon and oxygen (and potentially some nitrogen and hydrogen) leading to new atmospheric masses onto capturing terrestrial planets between that of the Earth's atmosphere to planets with massive atmospheres with sub-Neptune-like pressures. New secondary atmospheres with high metallicities will be created on terrestrial planets bathing in these late gas disks, resetting their primordial compositions inherited from the protoplanetary disk phase, and providing a new birth to planets that lost their atmospheres to photoevaporation or giant impacts. This volatile delivery for tens of Myr may also be favourable to the development of the first bricks of life. It will also affect the metallicity and C/O ratio of giant planets accreting late gas, which is an effect that may be observable in the close future. This very efficient accretion opens the way to a new planet detection method (for planets down to Earth masses at a few au from their stars) that I will present in this talk.
Janus: A NASA SIMPLEx mission to explore two NEO Binary Asteroids
Authors: Scheeres Daniel , McMahon Jay , Bierhaus Edward B. , Wood Joshua , Benner Lance , Hartzell Christine , Hayne Paul , Hopkins Joshua , Jedicke Robert , Le Corre Lucille , Naidu Shantanu , Pravec Petr , Ravine Mike
Published: October 2020

Janus is a NASA SIMPLEx mission currently in Phase B. The SIMPLEx program is designed around the idea of using secondary launch opportunities to explore interplanetary destinations. The Janus mission concept plans to take advantage of the NASA Psyche launch to send two spacecraft to fly by Near Earth Objects of interest. A specific point design has been developed that sends two spacecraft to two binary asteroid systems, (175706) 1996 FG3 and (35107) 1991 VH, both of which have been observed repeatedly with photometry, spectrometry and radar. The Janus mission sends light-weight, low-cost spacecraft built by Lockheed Martin to encounter these high-science value small body targets. The science instruments are a visible and IR imager, from Malin Space Science Systems. The spacecraft will perform a rigorous remote sensing campaign when the object is a point source, and when resolved. The spacecraft will track the binary asteroid systems through closest approach, allowing for a combination of absolute surface resolution, relative resolution across the target asteroids and phase angle coverage unparalleled in previous asteroid flyby missions. Janus science will combine flyby observations of the target binary asteroids with ground-based observations, enabling the high resolution imaging and thermal data to be placed into a global context and leveraging all available data to construct an accurate topographical and morphological model of these bodies. Based on these measurements, the formation and evolutionary implications for small rubble pile asteroids will be studied. The science team members all have experience on asteroid missions or have made extensive ground based observations of NEAs. The industry team has extensive experience in the design, fabrication and operation of interplanetary spacecraft and instrumentation.Acknowledgements: The Janus mission is supported by NASA under a contract from the SIMPLEx Program Office. Part of this research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.
Geographic diversity in Earth and Space sciences - do virtual conferences change the picture?
Authors: Dósa Melinda , Matenco Liviu , Heward Anita
Published: October 2020

In order to build a diverse, inclusive community of Earth and space scientists within Europe, a statistical study is carried out based on participation statistics of different conferences in Europe over the past five years. Data of geoscience conferences (EGU, IUGG), planetary (EPSC) and solar-terrestrial science conferences (ESWW, ESPM) are investigated. Special focus is given to the historical division between Eastern and Western Europe. The registration statistics of virtual conferences are also analysed.The aim is to show that the geographical division continues to exist and does not show a general improving trend, while the position of the younger generation seems to improve. Some “success cases” defying the usual trend are shown and analysed in detail. We suggest some reasons behind the statistics and draw some lessons that can help integrating less represented researchers into the mainstream of European Earth and space sciences.
ExPRES Modeling of Auroral Radio Source Occultation observed by Galileo Application to JUICE and Juno
Authors: Cecconi Baptiste , Louis Corentin K , Munoz Claudio , Vallat Claire
Published: October 2020

The ExPRES code simulates exoplanetary and planetary auroral radio emissions. It could be used to predict and interpret Jupiter’s radio emissions in the hectometric and decametric range. In this study, we model the occultations of the Jovian auroral radio emissions during the Galilean moons flybys by the Galileo spacecraft. In this study, we focus on auroral radio emissions, configuring the ExPRES simulations runs with typical radio source physical parameters. We compare the simulations run results with the actual Galileo/PWS observations, and show that we accurately model the temporal occurrence of the occultations in the whole spectral range observed by Galileo. We can then predict auroral radio emission occultations by the Galilean moons for the Juno and JUICE missions. ExPRES will be used by the JUICE/RPWI (Radio Plasma Waves Investigation) team to prepare its operation planning during the Galilean moon flybys for, e.g., the Galilean moon ionosphere characterization science objective, with passive ionospheric sounding during ingress and egress of Jovian radio source occultations. 
Refined study of the structure of the quasiperpendicular supercritical Martian shock: new results and methodology
Authors: Burne Sofia , Bertucci Cesar , Mazelle Christian , Morales Laura , Meziane Karim , Espley Jared , Halekas Jasper , Mitchell David , Penou Emmanuel
Published: October 2020

The study of the structure of the Martian shock is crucial to understand its microphysics and it is of special interest to understand the solar wind interaction with an unmagnetized, atmospheric body. The Martian bow shock is a rich example of a supercritical, mass-loaded, collisionless shock and it is one of the smallest of the solar system (both in absolute size and in terms of the solar wind ion gyroradii, of the same order of the curvature radius). This raises questions related to which particle acceleration and energy dissipation mechanism can take place, when its small size means dissipation timescales are too long for a stationary shock to convert the excess kinetic energy into heat. In addition, this shock coexists with ultra-low frequency (ULF) upstream waves, that are generated from the pick-up of exospheric ions.  We use MAVEN plasma and magnetic field data to show that the fine structure of the Martian supercritical quasi-perpendicular shock (given by the typical supercritical substructures: the foot, ramp and overshoot) is in many ways comparable with that of the Terrestrial shock, which presents a substantially different solar wind – planet interaction. We observe a shock foot of the order of an upstream ion convected gyroradius, that agrees with the model of specular reflection of foot formation (Woods, 1971; Livesey et al., 1984; Gosling and Thomsen, 1985). Also, we find that the shock ramp is typically very narrow, of the order of a few electron inertial lengths. The presence of a well-defined foot and overshoot confirm the importance of dissipative effects, even in such a small bow shock boundary. In this work we also provide a meticulous analysis methodology that stresses the importance on the correct processing of MAVEN data, and the clarity and consistency of the criteria used in the data selection and analysis. We pay special attention to the determination of the external limit of the entry to the ion foot and the identification of the main and secondary overshoots, where the presence of the ULF waves could mean an erroneous identification of these shock features. We also attempt to assess the non-stationarity of the shock substructures, even with the limitations of a single spacecraft mission, by computing a range of local shock speeds to obtain the substructures spatial widths from the timeseries within an upper and lower value. 

 

 
Interaction-Induced Dipole Moments of Carbon Dioxide
Authors: Beil Randi , Hinde Robert
Published: October 2020

The infrared absorption spectrum of carbon dioxide-rich planetary atmospheres, such as Venus or ancient Mars, can be difficult to model due to the presence of collision-induced absorption (CIA) features. These features appear in the 0-250 cm-1 region and are caused by the interaction-induced (I-I) dipole moments of carbon dioxide dimers. Studying these I-I dipole moments can lead to more accurate atmospheric models, which may then be used to create better estimates of the surface temperature of these planets thus revealing information about their climates either now (for Venus) or in the ancient past (for Mars).To investigate the I-I dipole moments of CO2 dimers, a finite-field approach was used to calculate the response properties of a carbon dioxide monomer, along with the energies and dipole moments of a T-shaped CO­2 dimer as a function of the intermolecular distance. Using the monomer results as fitting parameters, functions modeling these dipole moments were developed and compared to an analytically developed equation by M. S. A. El-Kader and G. Maroulis [1]. The resulting models for the I-I dipole moments presented here are thus based on purely ab initio results and are independent of any experimental variables.The response properties of the carbon dioxide monomers and the energies and dipole moments of the CO­2 dimers were calculated using the GAMESS-US ab initio software program and the NWChem ab initio software program. The I-I dipole moment equations were developed using the aug-cc-pVTZ basis set at the RHF, MP2, CCSD, and CCSD(T) levels of theory and the aug-cc-pVQZ and aug-pc-3 basis sets at the RHF and MP2 levels of theory. We have, to the best of our knowledge, reported the first purely ab initio I-I dipole moment model of a CO2 dimer. The resulting functions had a maximum absolute error below 10-3 au as shown in Figure 1, indicating that the functions provide an accurate description of the ab initio I-I dipole moments.References:1. El-Kader, M. S. A.; Maroulis, G. Chem. Phys. Lett. 670, 95-101 (2017) 

 
COVID-19 Dashboard Experiences – Lessons learned
Authors: Buziek Gerd
Published: October 2020

Abstract. As of March 2020, Esri Germany administers the Berlin based Robert Koch-Institute official COVID-19 Dashboard (Figure 1). During Esri’s evolvement both, organizational and technical processes have had to be built from scratch. Our objective was to keep society, as well as the disaster response units 24/7 informed about the spatiotemporal patterns of Corona pandemic. To achieve this several challenges had to be overcome. These challenges ranged from data gathering to data dissemination, from the delivery of COVID-19 information to the general public, as well as to the crisis prevention teams, and from the communication to individuals as well as to various specialists such as data journalists. Having a COVID-19 dashboard online results in a lot of publicity to the provider, but also requires a lot of effort to deliver a reliable and sustainable COVID-19 service, as many external decision making processes depend on the dashboard and the data which drives it. This presentation is not only about how we provided this service but will also include a look at the lessons learnt and how we can be best prepared for future spatiotemporal phenomena to help crisis response and perhaps even prevention.
Upgrade of existing algorithms for creating contour lines on topographic maps of the karst surface
Authors: Komel Neža Ema , Kozmus Trajkovski Klemen , Petrovič Dušan
Published: October 2020

Abstract. Today, many software tools enable the production of contour lines from relief models, but the results of modelling complex karst relief are often inadequate. Reasons for this may be limited quality and resolution of relief models, limitations of algorithms for calculating contours, or limitations of algorithms for smoothing and displaying additional symbols that further describe relief, such as slope lines, steep slopes and smaller objects that cannot be effectively displayed with contours, etc.We will present research in the field of improving existing algorithms in rugged karst terrain. As a target result, the presentation of relief on the existing national topographic maps in Slovenia, which were made by manual photogrammetric survey of aerial photos stereo pairs, were used. Slovenian elevation model DMR1 (1 m density) is used as a source for the creation of contour lines in various commercial software packages, and by comparing the results with a relief presentation on a topographic map, we selected the most appropriate basic algorithm. This one is further upgraded mainly by enabling automatic selection of auxiliary contour lines in the area, presentation of individual smaller relief objects with appropriate point or linear symbols, addition of slope lines on contours and indications in the middle of depressions and displacement of contour lines in order to better depict the terrain morphology.The results were tested in four different areas in Slovenia. Figure 1 shows the contour lines for a testing area near village Opatje Selo near Slovenia-Italy border, which were made by the best commercial software. The results of the algorithm are shown in Figure 2. The comparison between the results of the algorithm and the national topographic maps in the chosen scale gave promising results. In future work, we are planning to extend the algorithm so that it will be able to provide modelling of different terrains in the region.
Cartography Through the Years – Personal Views About a Young Science
Authors: Kainz Wolfgang
Published: October 2020

Abstract. Although cartographic products have been produced for thousands of years, cartography as a science has only been established in the early 20th century. Great works of cartography include, for instance, the conic map projections by Ptolemy, the Tabula Rogeriana by Idrisi, the Waldseemüller map, and the Mercator map. Numerous cartographers, predominantly mathematicians, have shaped the theory of map projections throughout the centuries.With the advent of geographic information systems (GIS) in the 1960s and the rapid developments of digital technologies, cartography found itself in the middle of an identity crisis. For some time, it was not clear whether cartography would become obsolete and be replaced by GIS mapping technologies or whether GIS is a novel manifestation of cartography. During this period various misconceptions about the role of maps and mapping as well as uncertainty about the future developments of mapping in general added to this confusion.This contribution elaborates the major characteristics of cartography versus other disciplines, in particular geography and GIS, and takes a look at possible future directions and developments with regard to the theory of cartography as well as novel and future display technologies. Personal observations of the author during his professional life since the early 1980s illustrate these developments.
Cartographic Visualisation of Spatial Phenomenons within Creative Industries
Authors: Netek Rostislav
Published: October 2020

Abstract. The paper discusses the issue of spatial visualisation within the topic of cultural and creative industries. Phenomenons such as spatial distribution, spatial evaluation of influence cultural subjects to the city environment, brain-drain and brain-gain of actors involved in the creative industries are demonstrated on the example of the Olomouc region, Czech Republic. It is based on spatial mapping of the creative industries in the region during the last decade. Based on the identification and collection of spatial data, over 1200 active subjects were identified in both spatial and non-spatial database. The general goal of the research is the find out the motivations of actors and talents within creative industries to leave from (brain-drain) or to come into (brain-gain) Olomouc region.The article focuses on the proposal of a strategy for strengthening the segment especially by spatial analysis and visualisation of the phenomenons. It aims to identify brain drain – talent and capital exodus with a purpose to propose stable position of creative industries within the region. The set of proposed measures and recommendations are primarily based on geographic and geoeconomic analyses supported by cartographic outputs. It offers to municipalities applicable tools to reduce side effects and identification of creative hubs, it enables systemic measures for recruitment and improvement of conditions for human capital development and acquisition. The presented paper describes the cartographic methods, procedures, spatial analyzes and map outputs achieved during the research.
Student’s Reading of Thematic Maps from Czech School World Atlas – an Eye-tracking Study
Authors: Beitlova Marketa , Popelka Stanislav , Vozenilek Vit
Published: October 2020

Abstract. According to the cartographic communication models, the map is intended as a product which helps people to understand the world. Usually, the first systematic cartographic product which pupils and students met in their lives is a school world atlas. In the Czech Republic, these atlases are used in almost every geography lesson. Thus, school atlases should be understandable, well-arranged, intelligible and easy to use by students. However, almost no empirical studies focused on this type of product exist.This presentation summarizes the results of the experiment, where the task was to find some object on the thematic map. The research aimed on two main issues: if the students are able to read thematic maps from school world atlas (Q1) and if the used cartographic visualization methods are properly selected (Q2).For finding answers to these research questions, the eye-tracking study conducted on 30 grammar school students was performed. This study contained ten tasks on the thematic world maps from the Czech school world atlas. Depending on the type of information displayed, visualization method and legend style, the tasks were formulated for each map. Eyemovement data were recorded using low-cost GazePoint eye-tracker with sampling frequency of 60 Hz. The first research question – if students can work with the thematic maps from school world atlas – was analysed using the correctness of answers and Trial Duration – the metric that shows how much time respondents needed to find the answer. For answering the second research question – if the cartographic methods used in the atlas are understandable –qualitative data visualization methods were used.At the beginning of the recorded data analysis, the correctness of answers and trial duration was ïnvestigated. These results helped us to find out, how the students were able to read the maps, if their answers were correct and how much time they needed for task solving. The results showed that generally, the students could read thematic maps (Q1). The most problematic task was the one where students had to estimate the pie-chart value according to the logarithmic scale.In the next step, the behaviour of students while solving each task was qualitatively described and problematic cartographic visualization methods were identified (Q2). For example, in some cases, used symbols were difficult to distinguish. The most serious problems were in the task, where students had to estimate the value of the bar chart. The scale of the legend was designed so that one millimetre of the bar corresponds to 50 million USD of export volume. This cartographic method was hard to understand for the students.The conducted eye-tracking study pointed out to maps where the cartographic methods were misused and caused problems to the students. The results might help the cartographers and map publishers who can modify the maps to be more understandable for the readers.
Current Challenges in Atlas Cartography
Authors: Sieber René , Losang Eric
Published: October 2020

Abstract. After decades of prosperity, atlas producers are faced with a serious number of challenges. Those challenges are both external and internal, either due to shifted external conditions or because of internal shortcomings. Internal challenges include, inter alia, the missing Web presence and PR, traditional atlas concepts, static GUI design, an overload of atlas features, default atlas contents, and repetitive visualization, whereas external influences, such as user behaviour, technological advancement and content that reflects new ideas and methods intensify these challenges.Three provocative statements – 1) atlases as mere collections of maps, 2) atlases rely on old-fashioned concepts, and 3) atlas map design is unattractive – are then picked in order to demonstrate possible approaches in rejuvenating atlas concepts.