bluuebunny/crossref_metadata_2025 huggingface dataset:
PENGARUH PELATIHAN DAN BEBAN KERJA TERHADAP KINERJA POKJA DI LINGKUNGAN BIRO PENGADAAN BARANG DAN JASA PEMERINTAH PROVINSI LAMPUNG
Authors: Tilaar Andy Fitriyadi Dharma
Published: October 2020

This study aims to determine the effect of Training, Workload, and Performance of Pokja di Lingkungan Biro Pengadaan Barang dan Jasa Pemerintah Provinsi Lampung. This phenomenon attracts the author's interest to further research and study by examining and analyzing "The Effect of Training and Workloads on the Performance of Pokja di Lingkungan Biro Pengadaan Barang dan Jasa pemerintah Provinsi Lampung” The focus of the study is on the concepts of Training, Workload, and Employee Performance. This type of research used for this thesis is evaluative research. Evaluative because this research is directed at testing the model. Arikunto, (2012) Based on the results of the analysis together - Leadership and Commitment affect the Performance with a calculated F value of 121,311 which means valid. Then in the t test conducted to see the magnitude of the influence of the individual independent variables on the dependent variable. The estimation results we can see that the calculated t-value for variables (X1) is 15,508 (Prob.sig. = 0,000) and for variables (X2) of -13,645 (Prob.sig. = 0,000) which means t-arithmetic> t-table with significance level of 95% (percent). Then the coefficient of determination of 83.8% (percent) of the variation in the effect of changes in training and workload can explain performance.

Keywords: Competencies, Work Experience, Human Resources Quality.

Penelitian ini bertujuan untuk mengetahui pengaruh Pelatihan, Beban Kerja, dan Kinerja Pokja di Lingkungan Biro Pengadaan Barang dan Jasa Pemerintah Provinsi Lampung. Fenomena ini menarik minat penulis untuk meneliti dan mengkaji lebih lanjut dengan cara menguji dan menganalisis “Pengaruh Pelatihan dan Beban Kerja Terhadap Kinerja Pokja di Lingkungan Biro Pengadaan Barang dan Jasa pemerintah Provinsi Lampung”. Fokus penelitian pada konsep Pelatihan, Beban Kerja, dan Kinerja Pegawai. Jenis penelitian yang digunakan untuk tesis ini adalah penelitian evaluatif. Bersifat evaluatif karena penelitian ini diarahkan pada pengujian model. Arikunto, (2012) Berdasarkan hasil analisis secara bersama – sama Kepemimpinan dan Komitmen berpengaruh terhadap Kinerja dengan nilai F hitung sebesar 121.311 yang berarti sahih. Kemudian pada uji t yang dilakukan untuk melihat besarnya pengaruh secara individu variabel bebas terhadap variabel tak bebas. Hasil estimasi dapat kita lihat bahwa nilai t-hitung untuk variabel (X1) sebesar 15.508 (Prob.sig. = 0,000) dan untuk variabel (X2) sebesar -13.645 (Prob.sig. = 0,000) yang berarti t-hitung > t-tabel dengan tingkat signifikansi 95% (persen). Kemudian koefisien determinasi sebesar 83,8% (persen) dari variasi perubahan pengaruh Pelatihan dan Beban Kerja dapat menjelaskan Kinerja.

Kata kunci: Kompetensi, Pengalaman Kerja, Kualitas SDM
Interannual and seasonal variations in the aerosol optical depth of the atmosphere in two regions of Spitsbergen (2002–2018)
Authors: Kabanov Dmitry M. , Ritter Christoph , Sakerin Sergey M.
Published: October 2020

Abstract. In this work, hourly averaged sun photometer data from Barentsburg and Ny-Ålesund, both located on Spitsbergen in the
European Arctic, are compared. Our data set comprises the years from 2002 to 2018
with overlapping measurements from both sites during the period from 2011 to 2018. For more turbid periods (aerosol optical depth, AOD, τ0.5>0.1), we found that Barentsburg is typically more polluted than
Ny-Ålesund, especially in the shortwave spectrum. However, the diurnal
variation in the AOD is highly correlated. Next, τ was divided into a fine
and coarse mode. It was found that the fine-mode aerosol optical
depth generally dominates and also shows a larger interannual than seasonal variation.
The fine-mode optical depth is in fact largest in spring during the Arctic
haze period. Overall the aerosol optical depth seems to decrease (at 500 nm
the fine-mode optical depth decreased by 0.016 over 10 years), although
this is hardly statistically significant.
New Observations of Upper Tropospheric NO2 from TROPOMI
Authors: Marais Eloise A. , Roberts John F. , Ryan Robert G. , Eskes Henk , Boersma K. Folkert , Choi Sungyeon , Joiner Joanna , Abuhassan Nader , Redondas Alberto , Grutter Michel , Cede Alexander , Gomez Laura , Navarro-Comas Monica
Published: October 2020

Abstract. Nitrogen oxides (NOx ≡ NO + NO2) in the NOx-limited upper troposphere (UT) are long-lived and so have a large influence on the oxidizing capacity of the troposphere and formation of the greenhouse gas ozone. Models misrepresent NOx in the UT and observations to address deficiencies in models are sparse. Here we obtain a year of near-global seasonal mean mixing ratios of NO2 in the UT (450–180 hPa) at 1 ° x 1° by applying cloud-slicing to partial columns of NO2 from TROPOMI. This follows refinement of the cloud-slicing algorithm with synthetic partial columns from the GEOS-Chem chemical transport model. We find that synthetic cloud-sliced UT NO2 are spatially consistent (R = 0.64) with UT NO2 calculated across the same cloud pressure range and scenes as are cloud-sliced (“true” UT NO2), but the cloud-sliced UT NO2 is 11–22 % more than the "true" all-sky seasonal mean. The largest contributors to differences between synthetic cloud-sliced and “true” UT NO2 are target resolution of the cloud-sliced product and uniformity of overlying stratospheric NO2. TROPOMI, prior to cloud-slicing, is corrected for a 13 % underestimate in stratospheric NO2 variance and a 50 % overestimate in free tropospheric NO2 determined by comparison to Pandora total columns at high-altitude sites in Mauna Loa, Izaña and Altzomoni, and MAX-DOAS and Pandora tropospheric columns at Izaña. Two cloud-sliced seasonal mean UT NO2 products for June 2019 to May 2020 are retrieved from corrected TROPOMI total columns using distinct TROPOMI cloud products that assume clouds are reflective boundaries (FRESCO-S) or water droplet layers (ROCINN-CAL). TROPOMI UT NO2 typically ranges from 20-30 pptv over remote oceans to > 80 pptv over locations with intense seasonal lightning. Spatial coverage is mostly in the tropics and subtropics with FRESCO-S and extends to the midlatitudes and polar regions with ROCINN-CAL, due to its greater abundance of optically thick clouds and wider cloud top altitude range. TROPOMI UT NO2 seasonal means are spatially consistent (R = 0.6–0.8) with an existing coarser spatial resolution (5° latitude x 8° longitude) UT NO2 product from the Ozone Monitoring Instrument (OMI). UT NO2 from TROPOMI is 12–26 pptv more than that from OMI due to increase in NO2 with altitude from the OMI pressure ceiling (280 hPa) to that for TROPOMI (180 hPa), but possibly also systematic altitude differences between the TROPOMI and OMI cloud products. The TROPOMI UT NO2 product offers potential to evaluate and improve representation of UT NOx in models and supplement aircraft observations that are sporadic and susceptible to large biases in the UT.
Biomarker on Callisto
Authors: Kushwaha Rahul , Lo Jeniu , Cheng Bing Ming , Sekhar Raja , Mason Nigel , Sivaraman Bhalamurugan
Published: October 2020

Ozone (O3), regarded as a biomarker, has been observed on the icy satellites Ganymede [1a], Dione and Rhea [1b]. Presence of O3 on the icy surfaces of Ganymede, Rhea and Dione are due to energetic processing of oxygen-bearing molecules. Laboratory experiments had shown efficient synthesis of O3 in oxygen-bearing molecules such as COx, SOx and NOx. Most of the experiments used InfraRed (IR) spectroscopy to detect O3 [2a]. However, unambiguous O3 detection in planetary objects using IR signatures is difficult due to the presence of silicates. Therefore, the Hartley band of O3, 220 – 310 nm, was used to find O3 presence on icy surfaces [2b]. Apart from the three satellites of the outer Solar System, there may be other satellites that might harbour O3. UltraViolet (UV) spectrum of Callisto recorded by the HST was reported to show spectral signatures of SO2 [3]. Based on this observation, the irradiation experiments simulating SO2 ices on Callisto revealed the coexistence of SO2 and O3. The spectral signatures in the UV were found to extend from 220 – 310 nm with a broad peak 255 – 285 nm, clear indication of O3 embedded in the SO2 ice matrix. Here we will present the detailed analysis that suggests the presence of O3 on Callisto.   References: [1] Noll et al. [a] (1996) Science, 273, 341. & [b] (1997) Nature, 388, 45.[2] Sivaraman et al. [a] (2007)  ApJ, 669, 1414. & [b] (2014) Chem Phy Lett, 603, 33.[3] Noll et al. (1997) GRL, 24, 1139.
The peak frequency source of Saturn’s Kilometric Radiation
Authors: Lamy Laurent
Published: October 2020

Before to ultimately plunge into Saturn’s atmosphere, the Cassini spacecraft explored between 2016 and 2017 the auroral regions of Saturn’s magnetosphere, where rises the Saturn’s Kilometric Radiation (SKR). This powerful, nonthermal, radio emission analog to Earth’s Auroral Kilometric Radiation, is radiated through the Cyclotron Maser Instability (CMI) by mildly relativistic electrons at frequencies close to the local electron gyrofrequency. The typical SKR spectrum, which ranges from a few kHz to ~1MHz, thus corresponds to auroral magnetic flux tubes populated by radiosources at altitudes ranging from ~4 kronian radii (Rs) down to the planetary ionosphere.  During the F-ring orbital sequence, Cassini probed the outer part of both northern and southern auroral regions, ranging from ~2.5 to ~4 Rs altitudes, and crossed several SKR low frequency sources (~10-30 kHz). Their analysis showed that the radiosources strongly vary with time and local time, with the lowest frequencies reached on the dawn sector. They were additionally colocated with the UV auroral oval and controlled by local time-variable magnetospheric electron densities, with importants consequences for the use SKR low frequency extensions as a proxy of magnetospheric dynamics. Along the proximal orbits, Cassini then explored auroral altitudes below ~2.5 Rs and crossed numerous, deeper, SKR sources at frequencies close to, or within the emission peak frequency (~80-200 kHz). Here, we present preliminary results of their survey analysis. Understanding how the CMI operates in the widely different environments of solar system magnetized planets has direct implications for the ongoing search of radio emissions from exoplanets, ultracool dwarves or stars.
Photometric results of the long-term monitoring of the active asteroid (596) Scheila
Authors: Lin Zhong-Yi , Hsu Chen-Yen
Published: October 2020

(596) Scheila was observed to have an active appearance as a result of impact event in late 2010. In additional the coma feature, the shape of light curve had been found the difference probably fresh material or surface properties changed around the impact site. In this study, we present the results of our monitoring observations obtained in 2014 and 2019-2020. The mean values of the color indices (B−V = (0.75 ± 0.08)m, V−R = (0.45 ± 0.04)m, and R−I = (0.44 ± 0.09)m) agree well with the values for asteroids of the D-types. The rotation period of the asteroid estimated from photometric observations in 2014 is 15.8 ± 0.1 h. The shape of the light curve is similar as that found after impact event. Furthermore, we did not find any rotational color variability in B-V, V-R and R-I diagrams, meaning the observed surface in this observing period of 2019-2020 is homogeneous.
Ganymede’s magnetic footprint mapping: Modeling and HST observations
Authors: Promfu Tatphicha , Wannawichian Suwicha , Nichols Jonathan , Clarke John
Published: October 2020

In this work, the locations of observed Ganymede’s magnetic footprint were compared with the locations predicted by the magnetic field model under different plasma conditions. The shifts of Ganymede's magnetic footprint locations from average footpath given by Grodent et al. (2008) were analyzed. The average path is created from about 1000 images taken by instruments onboarded Hubble Space Telescope (HST). The position shifts indicate the variation of magnetic field line mapping from Ganymede to Jupiter’s ionosphere. The two sets of data from HST were analyzed to obtain the locations of Ganymede’s magnetic footprint in 2007 and 2016. For both sets of data, at longitude ranging approximately from 170° to 180°, we found that the locations were significantly shifted in poleward direction between 0.5° to 2° from the average footpath. Different from data in May 2007, the Ganymede’s magnetic footprint locations in May 2016 at longitude about 160° could possibly locate in equatorward direction. At orbital distance of Ganymede about 15 RJ, in Jupiter’s middle magnetosphere, there is strong influence of plasma, whose major source is Io’s volcanic eruptions. Thus, the variations of plasma resulting in the stretching of magnetic field lines affect the magnetic field mapping from Ganymede to ionosphere. Furthermore, based on the magnetodisc model, the hot plasma pressure anisotropy strongly influences the stretching of the field lines and the mapped locations of Ganymede’s footprint in ionosphere to be shifted in either poleward or equatorward directions. In this study, we detected both poleward and equatorward shifts in different observations, whose connection with the plasma environment in the middle magnetosphere awaits for further study.
Danakil Depression: a multi-sensorial experience
Authors: Cavalazzi Barbara , Tistoni Samantha , Altobelli Francesco , Heward Anita
Published: October 2020

The beauty of Earth is clear! Earth's aesthetic beauty lies in the patterns, shapes, colours and textures of the land, oceans, ice and atmosphere, and this is evident to both scientists and artists who are fascinated by discovery and hypothesis, bythe surreal and the sublime, and by sounds from barren environments.Enthralled by the extreme harsh nature of the Danakil Depression, an extreme landscape between volcanoes and salty deserts – considered one the most inhospitable places on Earth – and inspired by the intensity of the light and colours, and by the resilience of the Afar culture, the authors will explore the beauty of the Earth by combining visual and sonic artwork, science, image and sounds influenced by a trip to the Danakil Depression in 2017 sponsored by Europlanet, thereby creatively expanding the fields of inquiry interested in reflecting upon our planet Earth. Acknowledgement. We thank Dr. Hickman-Lewis for ideas exchange on the importance of the integration of science and art. This work is a contribution to Europlanet 2024 RI Horizon 2020 (grant No 871149).
The CHEOPS Guaranteed Time Observing Programme
Authors: Isaak Kate , Queloz Didier , Benz Willy
Published: October 2020

Launched on 18 December 2019, CHEOPS (CHaracterising ExOPlanet Satellite) is the first exoplanet mission dedicated to the search for transits of exoplanets by means of ultrahigh precision photometry of bright stars already known to host planets. It is the first S-(small) class mission in ESA’s Cosmic Vision 2015-2025, and a partnership between Switzerland and ESA, with important contributions from 10 other member states.CHEOPS will provide the unique capability of determining accurate radii for a subset of planets in the super-Earth to Neptune mass range, for which masses have already been estimated from ground- based spectroscopic surveys. It will also provide precision radii for new planets discovered by ground- and space-based transit surveys, including TESS. By combining known masses with CHEOPS sizes, it will be possible to determine accurate densities for these smaller planets, providing key insight into their composition and internal structure. By identifying transiting exoplanets with high potential for in-depth characterisation – e.g. those that are potentially rocky and have thin atmospheres - CHEOPS will also provide prime targets for future instruments suited to the spectroscopic characterisation of exoplanetary atmospheres. 80 % of the obsering time in the 3.5 year nominal mission lifetime on the satellite is dedicated to the Guaranteed Time Observing Programme defined by the CHEOPS Science Team. The remaining 20% is available to the Community through the ESA Guest Observers Programme, which comprises annual calls and a discretionary time component.    
In this second poster in a series of three,  we present an overview of the CHEOPS Guaranteed Time Observing Programme as  defined by the CHEOPS Science Team. 
ESA’s Hera mission to asteroid Dimorphos
Authors: Carnelli Ian , Martino Paolo , Escorial Diego , rugina Ana , Gil Jesús , Greus Heli , Valverde Alberto , Zuccaro Alessandro , Bonnafous Bastien , Muñoz Moya Carlos , Honvault Christophe , Perez Lissi Franco , Tzeremes Georgios , Khan Michael , Küppers Michael , Tourloukis Michail , Muñoz Pablo , Concari Paolo , Moissl Richard , Accomazzo Andrea
Published: October 2020

The Hera mission contributes to the international effort towards the validation of the kinetic impactor asteroid deflection technique by retrieving all the physical and dynamical properties of Dimorphos in order to validate numerical impact codes. In particular, Hera’s core objectives from the point of view of the deflection demonstration are the following:(i) Measuring the mass of Dimorphos to determine the momentum transfer efficiency from DART to the asteroid;
(ii) Investigating the crater in detail to improve our understanding of the cratering process and the mechanisms by which the crater formation drives the momentum transfer efficiency;
(iii) Observing subtle dynamic effects (e.g. libration imposed by the impact, orbital and spin excitation of the secondary) that are difficult to detect for remote observers;
(iv) Characterising the physical properties of Dimorphos (including size, shape, volume, density, porosity, size distribution of surface material) to allow scaling of the momentum transfer efficiency to different asteroids.
In addition, the Hera mission will allow the demonstration of two key technologies for future deep-space missions:(v) The use of CubeSats for multipoint investigations operated via an inter-satellite network link via Hera;
(vi) Autonomous visual-based navigation for very low altitude flybys over the surface of Dimorphos.
 The Hera spacecraft will launch in October 2024 onboard an Ariane 6 launcher with an 18-days launch window. The trajectory foresees a Mars swing-by in mid-March 2025 and the rendezvous phase with Didymos starting end-December 2026. Following the operationally safe capture sequence, the asteroid close-proximity operation phase will start from a gate position of about 30 km. Operations will continue for about 6 months and allow for detailed investigations of the Didymos surface down to few kilometres or less from the surface of Dimorphos depending on the performance of the onboard feature-tracking navigation system. The mission is currently in phase B2 with OHB System as prime contractor together with GMV, QinetiQ, Spacebel and OHB-I as core team members. The preliminary design review is schedules in October 2020. The paper will provide an overview of the mission together with its latest system and payload configuration.
NEODECS - presentation of improved service
Authors: Jasik Daniel
Published: October 2020

At 2017 and 2018 EPSC meetings we presented a functioning version of the NEO Data Exchange and Collaboration Service (NEODECS) which is theplatform enabling collaboration between NEO researchers. This tool is also open for other Small Solar System Bodies like MBAs, TNOs, etc. Observerscan use this service to store, exchange or publish data from their observations, seek collaborators, broadcast observing plans and offer freetelescope time. This tool has been recently updated, based on feedback from researchers. We included functions to save telescopes, offer free telescope time and search for telescope offers. We also improved the process with registration to be more user-independent: in previous versions the tool required administrative input. Another improvement is providing tooltips describing most important functions showed just by moving cursor over them in menu. To provide help to new users we created a Welcome Tour for newcomers not experienced with NEODECS. It is provided in form of instruction videos showing how to use the most important functions. The goal of this presentation is to show practical usage of the NEODECS tool and encourage observers to use it.
A re-assessment of the Kuiper belt size distribution for sub-kilometer objects
Authors: Morbidelli Alessandro , Nesvorny David , Bottke William , Marchi Simone
Published: October 2020

In this work we combine several constraints provided by the crater records on Arrokoth and the worlds of the Pluto system to compute the size-frequency distribution (SFD) of the crater production function for craters with diameter D≤ 10km. For this purpose, we use a Kuiper belt objects (KBO) population model calibrated on telescopic surveys, that describes also the evolution of the KBO population during the early Solar System. We further calibrate this model using the crater record on Pluto, Charon and Nix.  Using this model, we compute the impact probability of bodies with diameter d>2km on Arrokoth, integrated over the age of the Solar System, that we compare with the corresponding impact probability on Charon. Our result, together with the observed density of sub-km craters on Arrokoth's imaged surface, constrains the power law slope of the crater production function. Other constraints come from the absence of craters with 1
F, Cl and 'water' mineral-melt partitioning in a reduced, model lunar system: what does the ‘volatile’ content of lunar rocks tell us?
Authors: Bromiley Geoffrey D. , Potts Nicola J. , Brooker Richard A.
Published: October 2020

The presence of ‘water’ (H-related defects), F, Cl and other volatiles in mare basalts and associated lunar volcanic glasses implies that lunar magmas were variably volatile-bearing[1]. Mineral-melt partition coefficients for each species can, in theory, be used to calculate volatile contents of lunar mantle source regions for these magmas. However, available partitioning data is largely based on studies in model terrestrial systems. Aside from differences in composition, the lunar mantle likely had an oxygen fugacity (fO2) at least 2 log units lower than the Earth’s upper mantle[3] and was either at or near Fe-saturation[1]. fO2 can have a fundamental influence on ‘water’ speciation in silicate melts, with H2 and C-H related defects stabilised under reducing conditions, at the expense of (OH)-  defects which dominate in oxidising terrestrial conditions[4]. As such, partitioning data in model, reduced lunar systems is required to accurately interpret measured volatile contents in lunar materials.We have developed a novel experimental design which allows us, for the first time, to constrain mineral-melt volatile partition coefficients under lunar mantle conditions. Experiments were performed at 2-3 GPa, 1350-1500°C, and at fO2 of IW-5 to IW+2 log units, in a system based on an average Apollo green glass[1]. Near-liquidus experiments were run to constrain olivine- and pyroxene-melt partition coefficients (Dmin/melt) for water, F and Cl, using EPMA and SIMS data. As shown in Fig. 1, values of Dmin/melt are comparable to those from experiments in more oxidised, terrestrial systems. F (and possibly Cl) incorporation in pyroxene and olivine is correlated with trivalent cation (Ti3+, Al3+, Cr3+) content, suggesting coupled substitution mechanisms[5], and is also dependent on the extent of melt polymerisation. However, fO2 has little discernible influence on partitioning behaviour. This is consistent with infrared and Raman spectra which show that (OH)- defects are the dominant mechanism for water incorporation in both silicate melt and coexisting mineral phases, with only a small proportion of water present as H2 defects in the most reduced, highest pressure samples. Higher pressures can stabilise a greater proportion of ‘water’ as H2, although this is unlikely to be an important mechanism for water storage in all but the deepest parts for the lunar mantle, as noted in previous thermodynamic models [6].Partitioning data can be used to re-interpret volatile contents of lunar mantle source regions. A batch melting calculation with 4-8% partial melting of a lunar mantle cumulate of 50% olivine, 25% pigeonite and 25% orthopyroxene[7], based on volatile concentrations from olivine-hosted melt inclusions and lunar volcanic glass beads[7,8], implies a lunar mantle source region with 2-8 ppm F, 0.07-0.3 ppm Cl, and
Boundary Layer Characterization using Mini-TES observations from the Mars Exploration Rovers
Authors: Mason Emily , Smith Michael
Published: October 2020

The Mars Exploration Rovers (MER), Spirit and Opportunity, landed on Mars in 2004 just weeks apart. Using spectra from the Miniature Thermal Emission Spectrometer (Mini-TES), both rovers were able to sample the lowest 2 km of the vertical temperature profile of the atmosphere. During a single observation for Mini-TES, spectra were taken every two seconds with observations lasting up to 42 minutes. While results up to this point have averaged the spectra together to retrieve information on dust, water vapor and temperature, individual temperature retrievals are possible every two seconds and contain information on short timescale atmospheric fluctuations. These fluctuations are indicative of boundary layer behavior at each site. We have retrieved the vertical temperature profile from individual spectra and have used these profiles to assess boundary layer conditions at each rover location. We will present temperature profiles from individual retrievals and identify and characterize fluctuations within these profiles. We will also show the seasonal variation of these fluctuations over the first 1200 sols (nearly 2 Mars Years) for both Spirit and Opportunity rovers.
Understanding the key requirement and the conditions that sparked life on Earth and beyond:clues and new knowledges supporting MuGeRo hypothesis.
Authors: del Gaudio Rosanna
Published: October 2020

The aim of this work is to present and discuss the results of recent and ongoing wet and in silico laboratory experiments supporting Multiple Root Genesis (MuGeRo) hypothesis already proposed in search of approaches surrounding the mysterious primeval steps of life emergence on Earth and elsewhere in the Universe. There are and have been reported many theories on how the very first life began on Earth, and also on how life itself evolved, some even say that life might have arisen on Earth more than once, and since it is hard to prove or disprove them there is no fully accepted theory.Approaching the primordial step of life emerging and possibile evolutionary scenarios from nonliving-matter towards answering the fundamental question about when, where and how life was born on Earth I’ll discuss essential requirement for the first emergence of life on Earth and Earth-like planets. As examples of proto-metabolic reactions occurred in a pre-biotic hydrogel context and as a model for the emergence and early evolution of life on Earth, I'm proposing the self-organizing M4 materials, having a complex chemistry, that I’ve obtained from both some meteorites and terrestrial rocks and minerals. Moreover, they are certainly the result of several coordinated activities and only some of them can be attributed to the meteorite or terrestrial rock components.The results so far obtained could point a way towards understanding how Earth kick-started metabolism emerged on landmass that arose from Archean oceans rather than in the depths near a deep sea hydrothermal vent. This work puts forward also an evolutionary scenario that satisfies the known constraints by proposing that life on Earth emerged, powered by solar radiation because the M4 catalytic activities might be a primitive form of reaction network supporting abiogenic development of life on Earth or elsewhere in the Universe. This in addition the idea that microbial or virus or early forms of life were already present in our solar system at the time of Earth’s formation so that panspermia or abiogenesis results are not rival but two complementary theories.Concerning the role that minerals may have played in organizing organic matter rising towards life from supports to scaffolds or energy sources or molecular-level information. There are some hints concerning the role that some minerals may have played in organizing matter in its rise towards life, from simple supports to scaffolds, from energy sources to even maybe providers of molecular-level information.The work that remains to be done is huge is there an "interfacial" path from the disorganized complexity of prebiotic and "primitive-jam" to the functional systems that have been the precursors of life? To answer this question I hope soon to analyze with systems chemists the results already obtained and they will be obtained from new weighted experiments designed in scientific cooperation.
Atmospheric dynamics on terrestrial planets with eccentric orbits
Authors: Guendelman Ilai , Kaspi Yohai
Published: October 2020

The insolation a planet receives from its parent star is the main engine of the climate and depends on the planet's orbital configuration. Planets with non-zero obliquity and eccentricity experience seasonal insolation variations. As a result, the climate exhibits a seasonal cycle, with its strength depending on the orbital configuration and atmospheric characteristics. In this study, using an idealized general circulation model, we examine the climate response to changes in eccentricity for both zero and non-zero obliquity planets. In the zero obliquity case, a comparison between the seasonal response to changes in eccentricity and perpetual changes in the solar constant shows that the seasonal response strongly depends on the orbital period and radiative timescale. More specifically, using a simple energy balance model, we show the importance of the latitudinal structure of the radiative timescale in the climate response. We also show that the response strongly depends on the atmospheric moisture content. The combination of an eccentric orbit with non-zero obliquity is complex, as the insolation also depends on the perihelion position. Although the detailed response of the climate to variations in eccentricity, obliquity, and perihelion is involved, the circulation is constrained mainly by the thermal Rossby number and the maximum temperature latitude. Finally, we discuss the importance of different planetary parameters that affect the climate response to orbital configuration variations.
Saturn’s nightside ring current during Cassini’s Grand Finale
Authors: Provan Gabrielle , Bradley Tom , Bunce Emma , Hunt Greg , Cowley Stan , Cao Hao , Dougherty Michele , Roussos Elias , Tao Chihiro
Published: October 2020

During Cassini’s Grand Finale proximal orbits, the spacecraft traversed the nightside magnetotail to ~21 Saturn radii.  Clear signatures of Saturn’s equatorial current sheet are observed in the magnetic field data.  An axisymmetric model of the ring current is fitted to these data, amended to taken into account the tilt of the current layer by solar wind forcing, its teardrop-shaped nature and the magnetotail and magnetopause fringing fields.  Variations in ring current parameters are examined in relation to external driving of the magnetosphere by the solar wind, and internal driving by the two planetary period oscillations (PPOs) and compared with dawn and dayside regimes.  The relative phasing of the PPOs determines the ring current’s response to solar wind conditions. During solar wind compressions when the PPOS are in antiphase, magnetospheric storms are triggered and a thick partial ring current is formed on the nightside, dominated by hot plasma injected by tail reconnection.  However, during solar wind compressions when the PPOs are in phase, the magnetosphere shows only a ‘minor’ response and a partial ring current is not observed. During solar wind rarefactions an equatorial ‘magnetodisc’ configuration is observed in the dayside/dawn/nightside regions, with similar total currents flowing at these local times.  This partial ring current should close partly via magnetopause currents and possibly via field-aligned currents into the ionosphere.  During very quiet intervals of prolonged solar wind rarefaction, a thin current sheet with an enhanced current density is formed, indicative of a ring current dominated by cool, dense, Enceladus water group ions.
Exospheric Na distributions along the Mercury orbit with the THEMIS telescope
Authors: Milillo Anna , Mangano Valeria , Massetti Stefano , Mura Alessandro , Plainaki Christina , Alberti Tommaso , Aronica Alessandro , De Angelis Elisabetta , Ippolito Alessandro , Kazakov Adrian , Noschese Raffaella , Orsini Stefano , Rispoli Rosanna , Sordini Roberto , Vertolli Nello
Published: October 2020

The variability of Na exosphere of Mercury shows time scales from less than one hour to seasonal variations. While the faster variations, accounting of about 10-20% of fluctuations are probably linked to the planetary response to solar wind and Interplanetary Magnetic Field variability, the seasonal variations (up to about 80%) should be explained by complex mechanisms involving different surface release processes, loss, source and migrations of the exospheric Na atoms. Eventually, a Na annual cycle can be identified. In the past, ground-based observations and equatorial density from MESSENGER data have been analysed. In this study, for a better investigation of the exospheric Na features, we have studied the local time and latitudinal distributions of the exospheric Na column density as a function of the True Anomaly Angle (TAA) of Mercury by means of the extended dataset of images, collected from 2009 to 2013, by the THEMIS solar telescope. Our results show that the THEMIS images, in agreement with previous results, registered a strong general increase at aphelion and a dawn ward emission predominance with respect to dusk ward and subsolar region between 90° and 150° TAA. Unlikely other analyses, ours evidences a predominance of subsolar column density along the rest of Mercury’s orbit. An unexpected relationship between Northward or Southward peak emission and both TAA and local time is also evidenced by our analysis. This result seems to contradict previous results obtained from different data sets and it is not easily explained, thus it requires further investigations.
Astrometric observations of Near Earth Objects and Minor Planet Center
Authors: Sioulas Nick
Published: October 2020

NOAK Observatory, Stavraki (IAU code L02) Ioannina, Greece (nsioulas@hotmail.com)IntroductionIn this work, the astrometric observations of four asteroids will be presented which took place on 2019 from NOAK observatory located at Stavraki in Greece. The results and the procedure of submitting the measurements to MinorPlanetCenter will be discussed.AbstractAstrometry is the measurement of positions, parallaxes and proper motion of an astronomical body. Especially the astrometry of Near Earth Objects (NEO) demands great accuracy and the cooperation between the professional and amateur astronomers for better results. All these objects that need confirmation are listed in the Near Earth Object Confirmation Page (NEOCP) and in the Possible Comet Confirmation Page (PCCP) at the site of the Minor Planet Center (MPC). When an object is confirmed, then a Minor Planet Electronic Circular (MPES) is published, including observations, the observers details and the orbital elements of the object. Due to the high number of the objects that need confirmation is important to use all available telescopes to track them.My amateur observatory participates in the effort to record all these objects in the Solar System. The Observatory also conducts observations of various objects and other phenomena such as exoplanet transits contributing to the Ariel Space Mission with the Exoclock Project. However, the main goal of the observatory is to conduct asteroid and comet photometry and the methods, observations and results will be discussed in this presentation.The observatory is registered in IAU as L02, «NOAK Observatory, Stavraki», in the town of Ioannina, Greece.AcknowledgementsI would like to thank Anastasia Kokori and Angelos Tsiaras for encouraging me to publish my work and for their advice. References [1] Minor Planet Center: https://www.minorplanetcenter.net/[2] Astrometrica: http://www.astrometrica.at/[3] Roger Dymock: Asteroids and Dwarf Planets[4] Brian D. Warner: A Practical Guide to Lightcurve Photometry and Analysis[5] Project Pluto: https://www.projectpluto.com/[6] NEODyS-2: https://newton.spacedys.com/[7] Center for Near Earth Objects Studies: https://cneos.jpl.nasa.gov/
Atmospheric speciation of rocky planets from magma ocean outgassing
Authors: Lichtenberg Tim , Bower Dan J. , Hammond Mark , Boukrouche Ryan , Tsai Shang-Min , Sanan Patrick , Sossi Paolo A. , Pierrehumbert Raymond T.
Published: October 2020

The earliest atmospheres of rocky planets originate from extensive volatile release during one or more magma ocean epochs that occur during primary and late-stage assembly of the planet (1). These epochs represent the most extreme cycling of volatiles between the interior and atmosphere in the history of a planet, and establish the initial distribution of the major volatile elements (C, H, N, O, S) between different chemical reservoirs that subsequently evolve via geological cycles. Crucially, the erosion or recycling of primary atmospheres bear upon the nature of the long-lived secondary atmospheres that will be probed with current and future observing facilities (2). Furthermore, the chemical speciation of the atmosphere arising from magma ocean processes can potentially be probed with present-day observations of tidally-locked rocky super-Earths (3). The speciation in turn strongly influences the climatic history of rocky planets, for instance the occurrence rate of planets that are locked in long-term runaway greenhouse states (4). We will present an integrated framework to model the build-up of the earliest atmospheres from magma ocean outgassing using a coupled model of mantle dynamics and atmospheric evolution. We consider the diversity of atmospheres that can arise for a range of initial planetary bulk compositions, and show how even small variations in volatile abundances can result in dramatically different atmospheric compositions and affect earliest mantle geochemistry and atmospheric speciation relevant for surficial prebiotic chemical environments (5). Only through the lense of coupled evolutionary models of terrestrial interiors and atmospheres can we begin to deconvolve the imprint of formation from that of evolution, with consequences for how we interpret the diversity revealed by astrophysical observables, and their relation to the earliest planetary conditions of our home world.References
Global hybrid simulations of highly compressed magnetosphere events at Mercury
Authors: Aizawa Sae , André Nicolas , Modolo Ronan , Leblanc François , Werner Elisabeth , Génot Vincent
Published: October 2020

The highly compressed magnetosphere (HCM) events at Mercury observed by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft have been investigated using the global hybrid simulation LatHyS. The HCM events occur due to the interactions with coronal mass ejections (CMEs) or high-speed streams (HSSs) and previous studies indicate that not only the reconnection-driven erosion but also the induced currents in the inner core have an important role in the variation of the dayside magnetosphere of Mercury. However, the effects of the presence of planetary ions on Mercury’s system have not been well discussed. In this study, we mainly focus on the presence of planetary ions that are self-consistently produced from the exosphere by several ionization processes under extreme solar wind conditions and discuss their role on the structure and dynamics of Mercury’s magnetosphere.
Understanding the trans-Neptunian Solar system; Reconciling the results of serendipitous stellar occultations and the inferences from the cratering record.
Authors: Shannon Andrew , Doressoundiram Alain , Roques Françoise , Sicardy Bruno
Published: October 2020

The most pristine remnants of the Solar system's planet formation epoch orbit the Sun beyond Neptune, the small bodies of the trans-Neptunian object populations.  The bulk of the mass is in ~100 km objects, but objects at smaller sizes have undergone minimal collisional processing, with "New Horizons" recently revealing that ~20 km (486958) Arrokoth appears to be a primordial body, not a collisional fragment.  This indicates bodies at these sizes (and perhaps smaller) retain a record of how they were formed.  However, such bodies are impractical to find by optical surveys due to their very low brightnesses.  Their presence can be inferred from the observed cratering record of Pluto and Charon, and directly measured by serendipitous stellar occultations.  These two methods produce conflicting results, with occultations measuring roughly ten times the number of ~km bodies inferred from the cratering record.  We apply MCMC sampling to explore numerical evolutionary models of the outer Solar system to understand what formation conditions can reconcile the occultations and cratering observations.  We find that models where the initial size of bodies decreases with their semimajor axis of formation, and models where the surface density of bodies increases beyond the 2:1 mean-motion resonance with Neptune can produce both sets of observations.  We discuss the astrophysical plausibility of these solutions, and possible future observations tests of them.
Six observational pieces of evidence against corotation as the main cause for the aurora at Jupiter
Authors: Bonfond Bertrand , Yao Zhonghua , Grodent Denis
Published: October 2020

The Main Emissions are the most recognizable feature of the aurorae at Jupiter and they are responsible for roughly 1/3rd of the total emitted power. They form an ever-present and quasi-continuous ring of emission centered on the magnetic poles. The most widely accepted explanation for these auroral emissions involves a current system related to the corotation enforcement of the plasma in the Jovian magnetosphere. Models based on this theory explain many characteristics of the aurorae. However, recent observations from the NASA Juno spacecraft and the ESA/NASA Hubble Space Telescope, complemented by previous results from the NASA Galileo spacecraft, challenge this theoretical framework. In this presentation, we will review six specific sets of observations contradictory with expectations from the corotation enforcement theory:We will expose their implications for the modelling of the Jovian magnetosphere and aurorae and we will discuss promising paths forward. 
Exploring Non-LTE Effects in Exoplanet Atmospheres
Authors: Wright Sam
Published: October 2020

Great advances have been made over the last few decades in probing the atmospheres of extra-solar planets, enabling us to further constrain the conditions that exist on these worlds. When modelling these atmospheres however, the work done to date has assumed that the species present are in local thermodynamic equilibrium (LTE). However it is known, for instance on Earth, that non-LTE effects are present in planetary atmospheres and give rise to spectra that vary from the LTE case.Fast, high altitude jet streams in the atmospheres of hot Jupiters will produce shock regions where molecules may be found in non-LTE. Such effects are also likely in the upper atmospheres of planets barraged by solar flares, where the heavy stellar radiation drives the molecules to a state of non-LTE.  This poster presents a preliminary exploration into non-LTE effects in exoplanet atmospheres, showing the differences that arise in some notable molecular spectra due to these effects. This is achieved with the atmospheric retrieval framework TauRex 3, using custom cross sections generated with the ExoCross software’s capability to approximate non-LTE spectra via splitting the rotational and vibrational temperatures. An initial evaluation of the detectability of these differences by current and next generation space telescopes is presented through simulation with the PandExo package, showing forward atmospheric models with non-LTE variations clearly visible in spectra. It can be seen that the differences in spectra are resolvable, notably the absence of ‘shoulders’ in the case of the non-LTE water transmission models.
Atmospheric Escape Processes and Planetary Atmospheric Evolution: from misconceptions to challenges
Authors: Gronoff Guillaume , Arras Phil , Baraka Suleiman , Bell Jared M , Cessateur Gael , Cohen Ofer , Curry Shannon M , Drake Jeremy J , Elrod Meredith , Erwin Justin , Garcia-Sage Katherine , Garraffo Cecilia , Heavens Nicholas G , Lovato Kylie , Maggiolo Romain , Parkinson Chris D , Simon Wedlund Cyril , Weimer Dan R , Moore William B
Published: October 2020

The recent discoveries of telluric exoplanets in the habitable zone of different stars have led to questioning the nature of their atmosphere, which is required to determine their habitability. Atmospheric escape is one of the challenging problems to be solved: simply adapting what is currently observed in the solar system is doomed to fail due to the large variations in the conditions encountered around other stars. A better strategy is to review the different processes that shaped planetary atmospheres and to evaluate their importance depending upon the stellar conditions. This approach allowed us to show that processes like ion-pickup were a more important way to lose atmosphere at Mars in the past. We reviewed the different escape mechanisms and their magnitude in function of the different conditions. This led us to discover discrepancies in the current literature concerning problems such as the Xenon paradox or the importance of a magnetic field in protecting an atmosphere.This shows that one should be very careful before claiming the presence of an atmosphere on planets in the habitable zone of their M-dwarfs: new criteria such as the Alfven surface location with respect to the planet should be taken into account a-priori.Overall, the habitability of a planet should not be claimed only on by its location in the habitable zone but also after careful analysis of the interaction between its atmosphere and its parent star [Gronoff et al. 2020].   Gronoff, G., Arras, P., Baraka, S., Bell, J. M., Cessateur, G., Cohen, O., et al. ( 2020). Atmospheric Escape Processes and Planetary Atmospheric Evolution. Journal of Geophysical Research: Space Physics, 125, e2019JA027639. https://doi.org/10.1029/2019JA027639 
Discovery of Alfven waves planetward of the Rings of Saturn
Authors: Southwood David , Cao Hao , Hunt Greg , Shebanits Oleg , Dougherty Michele
Published: October 2020

Between April and September 2017 in the final stages of the Cassini Saturn Orbiter mission the spacecraft executed 22 orbits passing planetward of the innermost ring, the D-ring.  During periapsis passes on all these orbits oscillations were detected in the azimuthal magnetic field components on typical time scales from a few minutes to 10 minutes. We argue that the time-varying signals detected on the spacecraft are also primarily time-varying in the plasma frame.  Nonetheless, we show that nearly all signals exhibit a distinct spatial effect, namely a magnetic node near the effective field line equator.  The oscillations thus have a standing structure along the background magnetic field and it follows that they are field line resonances associated with Alfvén waves.  The form of the signals suggests that the local field line resonances are most likely pumped from global sources.  This is the first detection in a giant planet magnetosphere of a phenomenon known to be important at Earth.