bluuebunny/crossref_metadata_2025 huggingface dataset:
The effectiveness of Gender Equality Plans in public research centers: the example of the Instituto de Astrofísica de Andalucía
Authors: Passas-Varo María
Published: September 2022

The Instituto de Astrofísica de Andalucía (IAA) is the largest Astronomy Institute of the Consejo Superior de Investigaciones Científicas (CSIC). The creation of the Institute's Gender Equality Commission and the annual elaboration and approval of the Gender Equality Plan (GEP) of the IAA-CSIC since 2017 confirm the IAA support for inclusive initiatives in gender equality. In this presentation, I will show the effectiveness of the different GEPs over time, by analyzing the statistics segregated by gender of the main activities of the last years at IAA.
Non-LTE effects in atmospheres of warm and hot Neptunes: implications for the atmospheric mass loss
Authors: Kubyshkina Daria , Fossati Luca
Published: September 2022

The warm- and hot-Neptune-type planets are known to experience significant atmospheric mass loss and are easier to observe and characterize in comparison to terrestrial-like planets. They represent, therefore, interesting targets in the context of planetary atmospheric evolution and star-planet interaction. The majority of studies, however, employ hydrodynamic simulations relying on simplified approaches in describing photoionization processes, or, on the other hand, use high-level photoionization solvers not accounting for dynamical effects.
In this study, we aim to outline for which types of planets in the Neptune-like mass range the non-LTE effects become important (in particular - in terms of atmospheric mass loss) and to which extent the hydrodynamic effects (as adiabatic expansion) influence the theoretically predicted transmission spectra.
To achieve this goal, we combine our 1D hydrodynamic upper atmosphere model (Kubyshkina et al., 2018) with the latest version of the non-LTE photoionization and radiative transfer code Cloudy (Ferland et al., 2017), which accounts for ionization and dissociation, atomic level transitions and chemical reactions for the lightest chemical elements up to zink. Thus, the former is responsible for resolving the hydrodynamic outflow and the latter solves the realistic photoionization and heating of the planetary atmosphere. We verify this scheme by comparing our results for a dozen of the high profile planets with the predictions of Salz et al., 2016, which use a similar approach.
We apply this hybrid framework to model the upper atmospheres of a range of Neptune-like and terrestrial-like planets with masses between 1 and 50 Mearth, changing systematically the orbital parameters (and thus, equilibrium temperature), and the irradiation level from the host star. We find, that for the majority of warm and hot Neptunes, accounting for realistic non-LTE ionization/heating affects significantly the basic parameters of planetary atmospheres, predicting cooler, slower, and denser outflow compared to the predictions of the pure hydrodynamic model. The predictions of the hydrodynamic and hybrid models become closer at the highest levels of stellar radiation.
In turn, accounting for hydrodynamic effects, in particular for expansion cooling, considerably affects the predictions of Cloudy models, and is therefore important for the interpretation of observations.

 
Coming soon to a sky near you: notable naked-eye astronomical events 2022–2040
Authors: Jones Graham
Published: September 2022

What are the notable forthcoming astronomical events for “the person in the street”? We present a brief overview of notable eclipses, appulses, and other groupings involving the Moon and the naked-eye planets. We’ll also make use of some of our other databases to answer questions such as: what is the biggest solar eclipse in terms of population coverage?
The effect of stellar composition on nebular condensation
Authors: Sossi Paolo , Wang Haiyang
Published: September 2022

The volatility of an element is defined by its 50% condensation temperature (Tc50) from a nebular gas of Solar composition at 10-4 bar. However, the variability in compositions of extrasolar systems inferred from the spectroscopic measurements of their parent stars implies that the identity, abundance and sequence of condensing phases should deviate from that of our Solar System. Here we perform Gibbs free energy minimisation with FactSage over temperatures from 1723 K to 473 K and 10-4 bar total pressure to calculate the condensation sequence of 39 stellar compositions in the system H-C-O-Na-Mg-Al-Si-S-Ca-Ti-Fe-Ni that span the range from -0.4 to +0.4 dex. In accord with previous work, the C/O ratio of the gas plays a profound role in determining the mineralogy and order of condensing phases. Nebulae with 0.3 < C/O < 0.75 display broadly solar condensation sequences. Condensing nebulae with C/O > 0.75 exhibit strongly decreasing Tc50 of lithophile elements whose condensation reactions depend upon the availability of oxygen (Ca, Al, Si, Ti, Mg) relative to those whose condensation does not (Fe, Ni). This trend is progressively reversed at very high C/O ratios for elements that form stable carbides, namely, TiC (C/O > 0.9) and SiC (C/O > 0.95), causing a dramatic increase in the Tc50 of Ti and Si. The Tc50 of S jumps from ~650 K below C/O = 0.75 to ~1100 K above C/O = 0.75 due to the condensation of oldhamite (CaS) and plateaus at higher C/O. The Tc50 of Fe and Ni increase monotonically with Fe/H, and are fit to equations Tc50(Fe) = 87.3(Fe/H) + 682 (r2 = 0.999) and Tc50(Ni) = 88.7(Fe/H) + 696 (r2 = 0.999) valid for 7.08 < Fe/H < 7.95 and 0.3 < C/O < 0.95. As the C/O and Fe/H ratios are broadly correlated, only high metallicity stars are expected to produce nebula condensates whose compositions diverge drastically from those of our Solar System. Planets formed from these systems should be richer in Fe, Ni and S at the expense of Al and Ca.
Europa’s interaction with the Jovian magnetosphere: insights from the Galileo flybys
Authors: Cervantes Villa Juan Sebastian , Saur Joachim
Published: September 2022

Europa, the smallest of the Galilean moons, is embedded within Jupiter’s magnetosphere where a rapidly flowing plasma interacts electromagnetically with the moon’s atmosphere and its surface. The magnetic field in the plasma is also affected by Europa’s induced magnetic field in a subsurface conducting layer. Between 1996 and 2000, the Galileo spacecraft executed eight close ﬂybys of Europa for which magnetic field measurements were obtained. Since then, several numerical magnetohydrodynamic (MHD) models have been developed to examine the interaction between the rapidly flowing Jovian magnetospheric plasma and Europa and its atmosphere (e.g. Kabin et al. [1999], Schilling et al. [2007], Rubin et al. [2015], Harris et al. [2021]).

In this study, we investigate the large scale interaction of Jupiter’s magnetospheric plasma with Europa and its atmosphere with a single fluid MHD model. We apply the 3D multiphysics model ZEUS-MP, based on Duling et al. [2014], and also employed by Blöcker at al. [2016] to describe Europa’s interaction. Our model accounts for ion-neutral collisions, electron impact ionization, dissociative recombination, and electromagnetic induction in a subsurface water ocean. In particular, we prescribe Europa’s molecular oxygen atmosphere with a number of analytical models in which we consider several degrees of asymmetry of the atmosphere and the location of Europa along its orbit around Jupiter, and we constrain its composition with Hubble Space Telescope (HST) spectral images.

The resulting magnetic field is compared with measurements performed by the Galileo magnetometer. We present an analysis of the observations from the Galileo flybys taking into consideration the variable geometry of the trajectories. Our comparative study is used to further constrain properties of the moon’s atmosphere and to quantify the effects of their variability on the plasma interaction.
Prospects for a local detection of dark matter with future missions to Uranus and Neptune 
Authors: Zwick Lorenz , Soyuer Deniz , Bucko Jozef
Published: September 2022

Past years have seen numerous papers underlining the importance of a space mission to the ice giants in the upcoming decade. Proposed missions to Uranus and Neptune usually involve a ~10 year cruise time to the ice giants. In this phase, the spacecraft trajectories will mainly be determined by the configuration of massive bodies in the solar system. Interplanetary trajectories are monitored by recording Doppler shifts in the time series of the radio link between Earth and the spacecraft. The presence of dark matter (DM) affects the trajectory by introducing a small radial acceleration, which in turn reduces the velocity of the spacecraft over years of interplanetary travel. Additionally, bounds on the precession rate of ice giants could help constrain the local DM density and potentially rule out modified gravity scenarios.

We investigate the possibility of detecting the gravitational influence of DM in the solar system on the trajectory of prospective Doppler ranging missions to Uranus and Neptune, and also estimate the constraints such a mission can provide on modified and massive gravity theories via extra-precession measurements using orbiters around the ice giants.

The precision of these measurements is limited by the noise on the the two-way frequency fluctuation of the Doppler link. For the trajectory deviations, we developed a numerical procedure for reconstructing the influence of DM in the Doppler signal of thousands of simulated ice giant missions.

The noise improvements required to guarantee a local detection of dark matter in the early 2040s are realistic, provided they become one of the priorities during mission development.
A MAVEN case study of radial IMF at Mars: impacts on the dayside ionosphere
Authors: Fowler Christopher , Hanley Gwen , McFadden James , Halekas Jasper , Schwartz Steven , Mazelle Christian , Chaffin Michael , Mitchell David , Andersson Laila , Espley Jared , Ramstad Robin , Dong Yaxue , Curry Shannon
Published: September 2022

Mars is an unmagnetized planet meaning that it has no internally generated global dipole magnetic field; the solar wind interaction with Mars is thus highly dependent on upstream conditions that include the orientation of the Interplanetary Magnetic Field (IMF). This interaction controls the transfer of energy and momentum from the solar wind into the magnetosphere, ionosphere and atmosphere, driving structure and dynamics within each. The Mars-solar wind interaction has been studied in detail for “nominal” Parker Spiral IMF conditions, but few studies exist that investigate the interaction under less typical “radial IMF” conditions. We utilize in-situ measurements made by NASAs Mars Atmosphere and Volatile EvolutioN (MAVEN) mission during radial IMF conditions at Mars to identify several prominent features that arise during this interaction:

Highly disturbed magnetic and plasma conditions exist over the nose of the planet, which are reminiscent of foreshock like conditions and indicative of radial IMF.

Solar wind protons and alphas are observed to penetrate directly into the dayside ionosphere down to MAVEN periapsis altitudes (~230 km).

The magnetic pileup region (or magnetic barrier) forms deep within the dayside ionosphere, directly exposing significant heavy planetary ion densities above to the solar wind flow.

Planetary ions above the magnetic barrier are mass loaded by the solar wind flow, characterized by signatures consistent with VxB acceleration under near radial IMF conditions.

Thermal ion distributions in the ionosphere are observed to possess significant suprathermal energetic tails, suggesting that additional energization mechanisms are present that heat the cold ion core. Electron and ion temperatures are 2-10 times higher than average values that occur under more typical IMF conditions.

Significant erosion of the dayside upper ionosphere occurs and appears to drive substantial ion escape to space.
Two Martian years at Mars: Observations by NOMAD on ExoMars Trace Gas Orbiter
Authors: Vandaele Ann Carine , Daerden Frank , Thomas Ian R. , Depiesse Cédric , Erwin Justin , Flimon Zachary , Neary Lori , Piccialli Arianna , Ristic Bojan , Trompet Loïc , Viscardy Sébastien , Willame Yannick , Aoki Shohei , Gérard Jean-Claude , Villanueva Geronimo , Mason Jon , Patel Manish , Bellucci Giancarlo , Lopez-Valverde Miguel , Lopez-Moreno Jose Juan
Published: September 2022

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) 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). NOMAD performs solar occultation, nadir and limb observations dedicated to the determination of the composition and the structure of the Martian atmosphere.

TGO started its science phase in April 2018 and instruments have now been accumulating data for more than two Martian years. We will present selected results obtained by the NOMAD instrument covering the atmosphere composition with observations of several trace gases, dust, and clouds. 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, ozone vertical profiles, climatology and relation with water, airglow observations, detection of CO2 ice clouds, surface ices 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.

 
Ukrainian School of Planetary Polarimetry
Authors: Kolokolova Ludmilla , Sosonkin Mikhail , Levasseur-Regourd Anny-Chantal
Published: September 2022

Planetary community knows Ukraine as a country that has a prominent history of polarimetric studies of Solar system objects. Ukrainian planetary polarimetry has been counting since 1926 when academician M. Barabashov (Kharkiv) observed polarization of the Moon. It got a significant impetus in late 1950th since then concentrating in Kharkiv, Kyiv, and Crimea, and gradually moving its focus from polarimetric studies of Mars and Venus to comets and asteroids, at the same time keeping the leading role in the lunar polarimetry.  In parallel with building polarimetric instrumentation and observing, Ukrainian polarimetric school also has had notable achievements in theory, specifically in studies of planetary and cometary atmospheres and surfaces of the Moon and asteroids, and in laboratory studies of light scattering by particulate surfaces. The devastating events of this year made it impossible for the Ukrainian polarimetrists to participate in the EPSC meeting. This poster intends to compensate for their absence by describing the history of the Ukrainian Polarimetric School and reminding the planetary community about leading Ukrainian polarimetrists and their contribution to the polarimetry of small bodies.
Explaining transition disks without massive planets
Authors: Gárate Matías , Pinilla Paola , Birnstiel Til , Ercolano Barbara , Stammler Sebastian M. , Picogna Giovanni , Delage Timmy N. , Stadler Jochen , Franz Raphael , Andrews Sean , Miotello Anna
Published: September 2022

Transition disks are one of the enigmas of the planet formation process: These objects typically feature wide gaps in the dust component, along with deficit of NIR emission corresponding to a lack of small grains in the inner regions, but simultaneously require a gas rich inner disk capable of sustaining high accretion rates, and a high content of pebble sized grains to explain the emission detected in the millimeter continuum.
Massive planets of several Jupiter masses have been long proposed as an explanation for these objects. However, despite the efforts to find these giants, only one or two disks have confirmed detections of a planetary companion. We propose a new hybrid model that easily explain the properties of transition disks, by combining the contributions made by different research groups over the last decade in photoevaporation, dead zones, and dust trapping. In our model photoevaporation takes care of opening a cavity in the gas and dust component, while dead zones in the inner regions lead to long lived-inner disk, capable of sustaining the observed accretion rates during the photoevaporative dispersal process. Finally, dust trapped in moderate substructures (such as the ones caused by small Saturn mass planets) can explain the emissions found in the millimeter continuum, without imposing strong constrains on the planet location.
With our model we show that instead of invoking massive fine-tuned planets to explain all the transition disk properties, the different processes that occur in protoplanetary disks complement each other and naturally reproduce the transition disk observations. Then, perhaps the reason of why we don't find more hidden massive planets is, simply, because they are not there.
The debiased compositional distribution of Near-Earth Objects
Authors: Marsset Michaël , DeMeo Francesca , Burt Brian , Polishook David , Binzel Richard , Granvik Mikael , Vernazza Pierre , Carry Benoit , Bus Schelte , Slivan Stephen , Thomas Cristina , Moskovitz Nicholas , Rivkin Andrew
Published: September 2022

We report 491 new near-infrared spectroscopic measurements of 420 Near-Earth Objects (NEOs) collected on NASA’s IRTF in the context of MITHNEOS (PI: DeMeo). The measurements were combined with previously published data (Binzel et al. 2019) and bias-corrected for albedo variations to derive the intrinsic compositional distribution of the overall NEO population. We also investigated individual subpopulations coming from various escape routes (ERs) in the asteroid belt by use of the dynamical model of Granvik et al. (2018). The resulting distributions reflect well the compositional gradient of the asteroid belt, with decreasing fractions of silicate-rich (S- and Q-type) bodies and increasing fractions of carbonaceous (B-, C-, D- and P-type) bodies as a function of increasing ER distance from the Sun. The compositional match between NEOs and their predicted source populations validates dynamical models used to identify ERs and argues against strong composition change in the main belt between approximately 5 km and 100 m. An exception comes from the overabundance of D-type NEOs from the 5:2J and, to a lesser extent, the 3:1J and ν6 ERs, hinting at the presence of a large population of small D-type asteroids in the main belt. Alternatively, this excess may indicate spectral evolution from D-type surfaces to C and P types due to space weathering or point to preferential fragmentation of D-types in the NEO space. No further evidence for the existence of collisional families in the main belt, below the detection limit of current main-belt surveys, was found in this work.
Auroral electrons at Mars: upstream drivers and ionospheric impact
Authors: Xu Shaosui , Mitchell David , McFadden James , Fowler Christopher , Hanley Gwen , Weber Tristan , Brain David , DiBraccio Gina , Liemohn Michael , Lillis Robert , Halekas Jasper , Ruhunusiri Suranga , Mazelle Christian , Benna Mehdi , Andersson Laila , Curry Shannon
Published: September 2022

Discrete aurorae have been observed at Mars by multiple spacecraft, including Mars Express, Mars Atmosphere and Volatile EvolutioN (MAVEN), and most recently the United Arab Emirates’ Hope spacecraft.  Meanwhile, there have been studies on the source particle responsible for producing these detectable aurorae, that is accelerated electrons or hotter solar wind electrons (termed “auroral electrons"). By utilizing empirical criteria to select auroral electrons established by Xu et al. [2022], we conduct statistical analyses of the impact of upstream drivers on the occurrence rate and electron fluxes of auroral electrons. We find the occurrence rate is well organized and increases with upstream dynamic pressure and weakly depends on the interplanetary magnetic field strength. Meanwhile, the integrated auroral electron flux is somewhat insensitive to the upstream drivers. In the meantime, the auroral emission is not the sole effect of electrons impacting the collisional atmosphere. Auroral electrons are expected to cause significant ionization and enhance the plasma density locally. In this study, we also quantify the ionospheric impact of auroral electron precipitation, specifically the thermal ion (O+, O2+, CO2+) density enhancement, with MAVEN observations and also modeling. Our results show the ion density to increase up to 1-2 orders of magnitude at low altitudes.
Per Aspera ad Astra Simul - ERASMUS+ program supporting mobilities ofyoung astronomers from Spain, Czechia and Slovakia
Authors: Kabath Petr , Jones David , Garcia Rojas Jorge , Toth Juraj , Jakubik Marian , Janik Jan , Hanus Josef
Published: September 2022

We will present the opportunities of an ERASMUS+ strategic partnership KA2 funding schemes which we used to support (not only) early career researchers in astronomy. ERASMUS+ is a general funding scheme and we describe here one particular project funding education and international partnerhsip of institutions in astronomical research. Our first Erasmus program (2017-2020) was enabling mobilities of early career researchers between Spanish, Czech and Slovak institutes. The mobilities helped young researchers to gain experience with the modern instrumentation at Observatorio Roque de Los Muchachos at La Palma, Spain. Our program helped several young researchers to obtain tenure track position in astronomical research. We also obtained a continuation of the ERASMUS+ program for another period (2020-2023) which focuses on the development of careers of young researchers and helping them to become future faculty leaders. Furthermore, within the program we performed educational activites for children of various ages. This contribution will describe our programs and its aims and results. We will also share our experience with the application process and with the ERASMUS+ program itself. We will describe the opportunities the ERASMUS+ program is offering for the education in an astronomical research for non-university research institutions.
1000 planetary transits measurements published in ExoClock by an amateur astronomer
Authors: Jongen Yves
Published: September 2022

1000 planetary transits measurements published in ExoClock by an amateur astronomer

Yves Jongen

Observatoire de Vaison, Vaison la Romaine, France

Abstract :

The ExoClock collaboration aims at improving the ephemerides of exoplanets that will be future targets for the Ariel mission.  ExoClock was launched in September 2019 and counts over 140 participants from more than 15 countries around the world.

A participant to the ExoClock Collaboration, the author has measured and published in ExoClock more than thousand planetary transit curves. The experimental equipment is composed of two identical telescopes (Plane Wave CDK 17”) of 430 mm diameter. One telescope is in Rasteau, in the South of France. The other telescope is installed at “Deep Sky Chile”, a telescope hosting facility located in the Rio Hurtado valley in Chile, not far from the Cerro Tololo, Gemini South and the brand-new Vera C. Rubin (LSST) observatories.

The poster will describe the experimental setup and the optical performances obtained at both sites, analyzing the strengths and weaknesses of each setup. The range of stars that can be best observed with each system will be described.

The poster will describe also the software used for the data acquisition and processing, as well as the tactics used in data processing to maximize the probability to obtain clean transit curves.

For high brightness stars, that could easily cause saturation in the camera, two solutions are compared: a slight defocusing, or averaging 2 4 or 8 short duration exposures for each step of the light curve
Isolated effects of gravity on sediment fluxes and delta morphology
Authors: Braat Lisanne , Lamb Michael P.
Published: September 2022

Fluvial landforms on Mars are important because they indicate past liquid water. The landforms can provide information about past environmental and climate conditions and the potential for past life. Ancient fluvial sediment transport fluxes have been estimated for several channels on Mars. However, it is also important to understand the differences between sediment transport on Earth and Mars. Fluxes can differ significantly due to gravity, sediment density, lack of ecology and the possible presence of ice. Only when we understand the effects of such differences on sediment fluxes, we can apply and adapt knowledge of fluvial geomorphology on Earth to the surface of Mars. Additionally, such understanding will greatly improve the use of Earth analogues.

In this study, we isolate the effects of gravity on fluvial sediment transport with a 1D model of a simple static channel and a 2D depth-averaged numerical hydro-geomorphological model of a growing delta. The results show that sediment transport on Mars is more efficient than on Earth for the same water discharge, sediment distribution, and channel geometry. The 1D results show that mainly fine sediment is transported more efficiently on Mars, because the effect of gravity is stronger on suspended transport compared to bedload transport and bigger grains travel in suspension on Mars compared to Earth for the same boundary conditions. Because gravity affects fine and coarse sediment fractions differently, we also expect differences in geomorphology due to different ratios of sediment fractions and disparities in sediment sorting. We are exploring these morphological effects in our 2D delta model. Our preliminary results suggest that the lower gravity on Mars results in faster-growing deltas with lower slopes and wider channels. These results suggest that unexpected differences with Earth might also occur in the delta stratigraphy, which is important to realise when drilling for sediment samples in the search for biosignatures.

 
DNA Damage Protection for Enhanced Bacterial Survival Under Simulated Low Earth Orbit Environmental Conditions in Escherichia coli
Authors: Puig Jaume , Knödlseder Nastassia , Quera Jaume , Algara Manuel , Güell Marc
Published: September 2022

Some organisms have shown to be able to naturally survive environments which we consider extreme, including the Low Earth Orbit, or even Outer Space. These microorganisms have natural mechanisms to repair severe DNA damage, such as the caused by ionizing and non-ionizing radiation or extreme temperatures and pressures. Some examples are Deinococcus radiodurans, which proved to be capable of surviving in the Exposure Facility of the International Space Station (ISS) for up to three years, and tardigrade species, such as Ramazzottius varieornatus, which are some of the most resilient known organisms. In this study, performed at the Barcelona Biomedical Research Park in collaboration with Hospital del Mar, survival under simulated Low Earth Orbit environmental conditions was tested in engineered and wild-type Escherichia coli strains. Ionizing radiation resistance was enhanced by transforming the Dsup gene from R. varieornatus and two genes from D. radiodurans involved in DNA damage repair, RecA and uvrD. This enhancement, together with a directed evolution process, resulted in a significant increase in the surviving fraction of the E. coli strain protected with the Dsup gene after a high dose, up to 3000 Gy, of ionizing radiation exposure in the form of a continuous spectrum of X-ray photons. Additionally, the survival to wide ranges of temperatures and low pressures was tested for the same strains, revealing a lack of relevance of cell aggregation for survival under the mentioned conditions in contrast with the case of D. radiodurans. However, survival rates showed no enhancement for any of the new E. coli strains. In a new collaboration with the Subterranean Laboratory of Canfranc, both the absence of radiation and extreme levels of radiation will be further studied. Additionally, an extreme environments analogue for several environmental conditions will be built, allowing for more specific testing on a controlled environment. This research represents a first step in the creation of new bacterial strains engineered to survive severe conditions and adapting existing species for their survival in remote environments, like extra-terrestrial habitats. These species could pave the road for future human expeditions, helping develop environments hospitable to life. In addition, studying the efficacy and the functioning of the genetic mechanisms used in this study could be beneficial for fields such as ecological restoration and medical and life sciences engineering, addressing treatments and/or diseases caused or related to radiation and DNA damage. Space is believed to be the last frontier, but the truth is, we are still a frontier to ourselves.
The distribution of methane in Titan's atmosphere during northern spring from Cassini/CIRS observations
Authors: Houelle Mathilde , Vinatier Sandrine , Bézard Bruno , Lellouch Emmanuel
Published: September 2022

We present a study of the methane abundance in Titan's lower stratosphere. We analyzed spectra of Titan's atmosphere in the mid- and far-infrared region recorded by the Composite Infrared Spectrometer (CIRS) aboard the Cassini spacecraft with nadir geometry to determine the methane mixing ratio between 1 and 20 mbar range and its variations with seasons and latitudes.

Lellouch et al. (2014) analyzed CIRS observations recorded over the first part of the Cassini-Huygens mission, from August 2005 to June 2010, during Titan's northern winter and early spring. They showed that the methane mole fraction in Titan's atmosphere varies with latitudes from about 1.0% to 1.5%, which was unexpected as, due to its long chemical lifetime, CH4 is supposed to be homogenized by the atmospheric circulation.

The goal of this study is to analyze Cassini/CIRS data taken over the last part of the mission during northern spring and early summer (June 2010 to September 2017) in order to retrieve CH4 mixing ratio, vertical profiles of temperature and aerosols opacity at the 19 latitudes that we have selected. We analyzed spectra acquired by two focal planes of CIRS (FP1 and FP4) covering the spectral range from 10 to 600 cm-1 and from 1050 to 1500 cm-1, respectively. FP1 spectra include emission from CH4 pure rotational lines and FP4 spectra include the CH4 ν4 band centered at 1305 cm-1. We use an iterative process to determine the temperature profile from the tropopause (using the FP1) to the low stratosphere (using the FP4) by fitting the continuum of the FP1 spectra in the 70-150 cm-1 wavenumber range and the CH4 ν4 band in the 1200-1350 cm-1 range. The obtained thermal profile is used to retrieve the methane mole fraction by fitting their rotational lines in the 75-150 cm-1 range. We use the obtained value as a priori of a new iteration (retrieving the temperature profile and the CH4 mole fraction subsequently). Convergence is obtained after a few iterations.

We will present the derived CH4 mixing ratios during the northern spring and compare them with the results of Lellouch et al. (2014), which mostly focused on the northern winter. This will allow us to derive potential seasonal variations that could occurred after the global circulation overturning during the spring.

 

Reference :

- Lellouch et al. (2014). The distribution of methane in Titan’s stratosphere from Cassini/CIRS observations. Icarus 231, 323-337.
The ExoClock Project: an open integrated platform for maintaining the Ariel target ephemerides with contributions from the public 
Authors: Kokori Anastasia
Published: September 2022

The ExoClock Project (www.exoclock.space) is an open, integrated, and interactive platform, designed to maintain the ephemerides accuracy of the Ariel targets. Ariel is ESA's medium class space mission prepared for launch in 2029. The main aim of the mission is to characterise a large number of exoplanets to better understand their nature. ExoClock aims to provide transit mid-time predictions for Ariel by collecting all currently available data (literature observations, observations conducted for other purposes, both from ground and space) and by efficiently planning dedicated efforts to follow-up the Ariel targets. ExoClock is open to contributions from a variety of audiences professional, amateur astronomers, university students and industry partners aiming to make the best use of all available resources towards delivering a verified list of ephemerides for the Ariel targets before the launch of the mission. In this presentation the organisation and the current status of the ExoClock project will be described. In addition, strategies and tools that are used to enable open science will be presented. Finally, the results will be presented from almost three years of operation of the project. 
Methane vertical profile in Titan’s atmosphere
Authors: Gautier Thomas , Serigano Joseph , Das Koyena , Coutelier Maélie , Hörst Sarah , Vinatier Sandrine , Szopa Cyril , Trainer Melissa
Published: September 2022

More than a decade after the arrival of the Cassini-Huygens mission in Saturn’s system, data returned by the Huygens probe during its descent remain a unique source of in-situ information on the lower atmosphere of Titan. Among the Huygens instrumental suite was the GCMS (Gas Chromatograph Mass Spectrometer) instrument which returned hundreds of mass spectra acquired in the atmosphere below 145 km of altitude.

We will present a reanalysis of GCMS data focusing on the methane vertical profile thanks to recent advances in our knowledge of Titan’s atmosphere and in mass spectrometry data treatment [1-3].

We retrieved methane mixing ratio slightly lower than the one reported by the original team[4] and obtained its profile between 145 km and 30 km of altitude with a kilometric vertical resolution, and a sub-kilometric one between 30 km and the surface.

Such a vertical resolution unveiled clear oscillations in the methane mixing ratio in Titan’s troposphere and methane vertical concentration diverging from an ideal adiabat. Such features could for example be a sign of small-scale convective zones in the troposphere which could have triggered the gravity waves detected by Huygens in the stratosphere. We hope that the discovery of previously unnoticed features in GCMS data will also enable the reanalysis of data returned by other Huygens instruments such as HASI and DISR on Titan lower atmosphere.

[1] Gautier et al. Decomposition of electron ionization mass spectra for space application using a Monte-Carlo approach. Rapid. Com. Mass Spec. 34(8), e8659 (2020)

[2] Serigano et al. Compositional measurements of Saturn’s upper atmosphere and rings from Cassini INMS. JGR:Planets, 125 (8), E006427  (2020)

[3] Serigano et al. Compositional Measurements of Saturn’s Upper Atmosphere and Rings from Cassini INMS: An extended Analysis of Measurements from Cassini’s Grand Finale Orbits. JGR:Planets, 127, E007238 (2022)

[4] Niemann et al. Composition of Titan’s lower atmosphere and simple surface volatiles as measured by the Cassini-Huygens probe gas chromatograph mass spectrometer experiment. JGR 115, E12006, 2010
Blue biotopes in Icelandic lava tubes: analog environments for subsurface life on Mars
Authors: Kopacz Nina , Csuka Joleen , Baqué Mickael , Iakubivskyi Iaroslav , Guðlaugardóttir Hrefna , Klarenberg Ingeborg J. , Ahmed Mahid , Zetterlind Alexandra , Singh Abhijeet , ten Kate Inge Loes , Hellebrand Eric , Stockwell Brent R. , Stefánsson Árni B. , Vilhelmsson Oddur , Neubeck Anna , Anna Schnürer Anna , Geppert Wolf
Published: September 2022

Lava tubes on Mars hold exciting potential for the preservation of biosignatures, which may survive on geological timescales in these isolated, stable environments. To support the development of future astrobiological mission concepts, we turn to terrestrial lava tubes, host to a variety of microbial communities and secondary minerals. Following a multidisciplinary sampling protocol, we retrieved biological, molecular, and mineralogical data from several lava tubes in Iceland. We report on blue-colored copper-rich secondary minerals and their associated bacterial communities using a multi-method approach, and an amalgam of 16S rRNA gene sequencing, Raman spectroscopy, scanning electron microscopy, and energy-dispersive X-ray spectroscopy data sets. We found numerous bacterial genera known for their high metal resistance and ability to survive in low-nutrient environments. Both are characteristics to be expected for any potential life in Martian lava tubes, and should be considered when checking for contaminants in Mars mission preparations. Associated with the microbial mats, we identified several types of copper-rich secondary minerals, indicating localized copper enrichments in the groundwater, possibly stemming from overlying ash deposits and nearby hyaloclastite formations. Molecular analysis revealed carotenoid signals preserved within the copper speleothems. If found in Martian lava tubes, blue copper-rich mineral precipitates would be deserving of astrobiological investigation, as they have potential to preserve biosignatures and harbor life.
Application of a P-T dependent partition coefficient model to a 1D thermal evolution code of Mars
Authors: Schmidt Julia Marleen , Noack Lena
Published: September 2022

In partial melt zones, incompatible elements like the heat producing elements (HPE) K, Th, and U are redistributed from the solid to liquid material. If the melt is in an area where it is buoyant, it transports the incompatible elements towards the surface and leaves a depleted upper mantle area behind. Partition coefficients can act as a measure for the amount of the redistributed elements. They are highly sensitive to temperature, pressure, and composition and can change by multiple orders of magnitude along the peridotite solidus from 0-15 GPa (Fig. 1, Schmidt and Noack, 2021). However, since there is a lack of high-pressure models and experimental data, partition coefficients in mantle evolution models were generally taken as constant values.

Clinopyroxene is a common mantle material which takes up most trace elements and is therefore highly relevant for redistribution processes. Also, compared to other minerals that can be found in the upper mantle of Mars and Earth, clinopyroxene undergoes the largest changes of partition coefficients with changes in temperature and pressure. In clinopyroxene, sodium acts as a compatible element with partitioning behaviors similar to  incompatible trace elements, which is why it can be used as a reference for modelling other trace elements’ partition coefficients. In this study, we take the parameterization for the partitioning of sodium of Schmidt and Noack (2021) and calculate partition coefficients for HPE at local P-T conditions. This parameterization is derived from a thermodynamic model (Fig. 1) based on Blundy et al (1995) and valid for pressures up to 12 GPa. We apply these calculated partition coefficients to a 1D interior evolution model for Mars and compare the resulting HPE enrichments to the ones obtained with models using constant partition coefficients for variable initial conditions. By doing so, we can compare data obtained from Mars missions to our modelled approach and subsequently constrain the influence the varied parameters and the partitioning model have on the thermal evolution of Mars.

Fig. 1: Thermodynamic model for sodium partitioning in clinopyroxene/melt. Along the peridotite solidus,
the partition coefficients vary up to two orders of magnitude (Schmidt and Noack, 2021).

Schmidt, J.M. and Noack, L. (2021): Clinopyroxene/Melt Partitioning: Models for Higher Upper Mantle Pressures Applied to Sodium and Potassium, SysMea, 13(3&4), 125-136.

Blundy, J. et al. (1995): Sodium partitioning between clinopyroxene and silicate melts, J. Geophys. Res., 100, 15501-15515.
Venus Dynamics Tracer - exploring Venus with balloons
Authors: Stenberg Wieser Gabriella , Persson Moa
Published: September 2022

Venus Dynamics Tracer (VdT) is a proposal for a multi-balloon mission to Venus that was submitted as a response to the ESA call for new M-class missions. This presentation discusses the science questions that could be addressed using two balloons at different altitudes in Venus atmosphere together with an orbiter. The main goal of VdT is to reveal how the atmospheric motion in the Venus atmosphere is driven by the energy originating from absorption of solar radiation. VdT achieves this by in situ measurements in two major regions where driving “motors” are located: Firstly, the cloud layer where visible light is absorbed and drives the vertical motions of the air. Secondly, the upper atmosphere where EUV is absorbed both by neutrals and ions and where energy and momentum are transferred between them. VdT combines the in situ measurements by two balloons at different altitudes in the atmosphere with in situ and remote sensing observations from an orbiter. The mission aims to answer the following questions: 1. What are the roles of the vertical and meridional circulation in maintaining major atmospheric dynamics near the clouds, including the superrotation? and 2. What is the global dynamics of ions and neutrals in the upper atmosphere?

VdT has only 50 kg scientific payload but enables break-through science by a unique distribution of the payload: 40 kg on an orbiter and 5 kg each on two atmospheric balloons. The presentation describes and motivates the suggested payload.
Europlanet 2024 RI: Fostering the collaboration between professional and amateur astronomers
Authors: Tautvaisiene Grazina , Hueso Ricardo , Podlewska-Gaca Edyta , Kargl Guenter , Mikolaitis Sarunas , Garate-Lopez Itziar
Published: September 2022

The Europlanet 2024 Research Infrastructure (RI) provides free access to the world’s largest collection of planetary simulation and analysis facilities, data services and tools, a ground-based observational network and programme of community support activities (https://www.europlanet-society.org/europlanet-2024-ri/). 

A new collaboration between telescopes around the world has been launched in 2020 to provide coordinated observations and rapid responses in support of planetary research from space missions and in follow-ups of new events. The Europlanet Telescope Network (EPN-TN) is providing professional and trained amateur observers with access to small and medium-sized telescopes located around the globe (https://www.europlanet-society.org/europlanet-2024-ri/telescope-network/).

The EPN-TN currently comprises 16 observatories with 46 telescopes ranging from 40 cm to 2 m in size. The network can be accessed free of charge to carry out projects on a wide variety of scientific studies about the Solar System and exoplanets, as well as related astronomical investigations. The network is open for new infrastructures.

 The first scientific results achieved with EPN-TN were  presented at the Europlanet Telescope Network Science Meeting held on the 6-11 February, 2022. Among 210 participants from 43 countries, there were 80 amateur astronomers participating  (http://mao.tfai.vu.lt/europlanet2022/). The network aims to strengthen collaborations between professional and amateur astronomers, who are playing an increasingly important role in planetary research. Observing time applicants from amateur astronomers are very welcome. 

We will overview the EPN-TN and its potential in fostering the collaboration between professional and amateur astronomers.

Acknowledgements

Europlanet 2024 RI has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 871149.
Absolute photometry of the transneptunian dwarf planets in a long time span
Authors: Morales Nicolás , Ortiz José Luis , Morales Rafael , Fernández-Valenzuela Estela , Santos-Sanz Pablo , Duffard René , Kretlow Mike , Vara Mónica
Published: September 2022

We have analyzed our database with thousands of images including trans-Neptunian dwarf planets. This images have been obtained since 2005 within our own observing programs to derive absolute photometry at different wavelength bands. We have used specifically designed tools that take into account color terms to derive accurate photometric transformations by taking advantage of the latest Gaia EDR3 photometry [1] for the reference stars in our images. With this remarkable 16-year time span we derive accurate absolute magnitudes and phase slopes in order to analyse trends along the years. Our observing program has mainly used the 1.5-m telescope at Sierra Nevada Observatory in Spain and the 1.23-m telescope at Calar Alto Observatory in Spain but also includes other telescopes such us the TNG or the WHT at La Palma Observatory, Spain. Using some archive images we have also been able to extend the available time span.

We will present our preliminary analysis and results of the long term evolution of some of the physical properties for the dwarf planets Haumea, Makemake and Eris.

 

 

We acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709).
Funding from Spanish projects PID2020-112789GB-I00 from AEI and Proyecto de Excelencia de la Junta de Andalucía PY20-01309 is acknowledged. Part of the research leading to these results has received funding from the European Research Council under the European Community’s H2020 (2014-2020/ERC Grant Agreement no. 669416 “LUCKY STAR”). M.V-L. acknowledges funding from Spanish project AYA2017-89637-R (FEDER/MICINN). P.S-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 “LEO-SBNAF”.

 

[1] M. Riello , F. De Angeli , D. W. Evans et al. A&A 649, A3 (2021)