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1. Reflectivity of Venus' dayside disk during the 2020 observation campaign: outcomes and future perspectives

Author: Lee, Yeon Joo, Muñoz, Antonio García, Yamazaki, Atsushi, Quémerais, Eric, Mottola, Stefano, Hellmich, Stephan, Granzer, Thomas, Bergond, Gilles, Roth, Martin, Gallego Cano, Eulalia, Chaufray, Jean-Yves, Robidel, Rozenn, Murakami, Go, Masunaga, Kei s, Kaplan, Murat, Erece, Orhan, Hueso, Ricardo, Kabáth, Petr, Špoková, Magdaléna, Sánchez-Lavega, Agustín, Kim, Myung-Jin, Mangano, Valeria, Jessup, Kandis-Lea, Widemann, Thomas, Sugiyama, Ko-ichiro, Watanabe, Shigeto, Yamada, Manabu, Satoh, Takehiko, Nakamura, Masato, Imai, Masataka se, Cabrera, Juan, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Pioneer Research Center for Climate and Earth Science (PRC), Institute of Basic Science (IBS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Graduate School of Science [Tokyo], The University of Tokyo (UTokyo), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique [Versoix] (LASTRO), Ecole Polytechnique Fédérale de Lausanne (EPFL), Leibniz Institute for Astrophysics Potsdam (AIP), Centro Astronómico Hispano Alemán, Observatorio de Calar Alto (CAHA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofísica de Andalucía (IAA), Akdeniz University, Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Department of Theoretical Physics and Astrophysics [Brno], Masaryk University [Brno] (MUNI), Korea Astronomy and Space Science Institute (KASI), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Southwest Research Institute [Boulder] (SwRI), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Matsue National College of Technology, Hokkaido Information University, Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Kyoto Sangyo University, Ministerio de Ciencia e Innovación (España), and European Commission
Subjects: atmospheric clouds, fourier-transform measurements, Earth and Planetary Astrophysics (astro-ph.EP), sulfur-dioxide, uv absorption, solar system astronomy, FOS: Physical sciences, absorption cross-sections, Venus, cloud-top, valence-shell, observational astronomy, s 2p, planetary science, photoabsorption, [SDU]Sciences of the Universe [physics], temperature-dependence, carbonyl sulfide, planetary atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract: This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We performed a unique Venus observation campaign to measure the disk brightness of Venus over a broad range of wavelengths in 2020 August and September. The primary goal of the campaign was to investigate the absorption properties of the unknown absorber in the clouds. The secondary goal was to extract a disk mean SO2 gas abundance, whose absorption spectral feature is entangled with that of the unknown absorber at ultraviolet wavelengths. A total of three spacecraft and six ground-based telescopes participated in this campaign, covering the 52–1700 nm wavelength range. After careful evaluation of the observational data, we focused on the data sets acquired by four facilities. We accomplished our primary goal by analyzing the reflectivity spectrum of the Venus disk over the 283–800 nm wavelengths. Considerable absorption is present in the 350–450 nm range, for which we retrieved the corresponding optical depth of the unknown absorber. The result shows the consistent wavelength dependence of the relative optical depth with that at low latitudes, during the Venus flyby by MESSENGER in 2007, which was expected because the overall disk reflectivity is dominated by low latitudes. Last, we summarize the experience that we obtained during this first campaign, which should enable us to accomplish our second goal in future campaigns. © 2022. The Author(s). Published by the American Astronomical Society., This research used data collected at the Centro Astronómico Hispano-Alemán (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC). This research has made use of the integral field spectroscopy data reduction tool p3d, which is provided by the Leibniz-Institut für Astrophysik Potsdam (AIP). Akatsuki/UVI data are publicly available at the JAXA archive website, DARTS (http://darts.isas.jaxa.jp/), and the NASA archive website, PDS (https://pds.nasa.gov/). UVI Level 3 products (l3bx) were used in this study (Murakami et al. 2018). This study used the TSIS-1 SIM data (Version 06, doi:10.25810/y9f8-ff85). M.K. and O.E. thank the TÜBİTAK National Observatory for partial support in using the T100 telescope, with project number 20CT100-1688. R.H. and A.S.L. have been supported by the Spanish project PID2019-109467GB-I00 (MINECO/FEDER, UE) and Grupos Gobierno Vasco IT-1366-19. P.K. and M.S. acknowledge support from grant LTT-20015., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
Published: 2022
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2. Balmer continuum enhancement detected in a mini flare observed with IRIS

Author: Ramesh Chandra, Brigitte Schmieder, Reetika Joshi, James Tomin, Petr Heinzel, Nicole Vilmer, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: chromosphere, Sun: flares, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, 7. Clean energy, 01 natural sciences, Spectral line, law.invention, symbols.namesake, MAGNETIC RECONNECTION, law, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Sun: transition region, SOLAR, 010303 astronomy & astrophysics, Chromosphere, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Science & Technology, Solar flare, Astrophysics::Instrumentation and Methods for Astrophysics, Sun, Sun: chromosphere, Balmer series, Astronomy and Astrophysics, flares, Physics::History of Physics, Astrophysics - Solar and Stellar Astrophysics, transition region, Space and Planetary Science, Physical Sciences, X-RAY, symbols, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope, Flare
Abstract: Optical and near-UV continuum emissions in flares contribute substantially to flare energy budget. Two mechanisms play an important role for continuum emission in flares: hydrogen recombination after sudden ionization at chromospheric layers and transportation of the energy radiatively from the chromosphere to lower layers in the atmosphere, the so called back-warming. The aim of the paper is to disentangle between these two mechanisms for the excess of Balmer continuum observed in a flare. Methods. We combine the observations of Balmer continuum obtained with IRIS (spectra and SJIs 2832 A) and hard X-ray (HXR) emission detected by FERMI Gamma Burst Monitor (GBM) during a mini flare. Calibrated Balmer continuum is compared to non-LTE radiative transfer flare models and radiated energy is estimated. Assuming thick target HXR emission, we calculate the energy of non-thermal electrons detected by FERMI GBM and compare it to the radiated energy. The favorable argument of a relationship between the Balmer continuum excess and the HXR emission is that there is a good time coincidence between both of them. In addition, the shape of the maximum brightness in the 2832 SJIs, which is mainly due to this Balmer continuum excess, is similar to the FERMI/GBM light curve. The electron-beam flux estimated from FERMI/GBM is consistent with the beam flux required in non-LTE radiative transfer models to get the excess of Balmer continuum emission observed in the IRIS spectra. The low energy input by non thermal electrons above 20 keV is sufficient to produce the enhancement of Balmer continuum emission. This could be explained by the topology of the reconnection site. The reconnection starts in a tiny bald patch region which is transformed dynamically in a X-point current sheet. The size of the interacting region would be under the spatial resolution of the instrument., Comment: 10 pages, 11 figures, Accepted for publication in Astronomy and Astrophysics
Published: 2021

3. An advanced multipole model for (216) Kleopatra triple system

Author: Laurent Jorda, Josef Hanus, François Colas, Alexis Drouard, J. Grice, Julie Castillo-Rogez, Patrick Michel, Philippe Lamy, Pierre Vernazza, Josef Ďurech, Miroslav Brož, Bin Yang, Matti Viikinkoski, Franck Marchis, Tadeusz Michalowski, Marin Ferrais, Fabrice Cipriani, Thierry Fusco, Nicolas Rambaux, Olivier Witasse, Przemyslaw Bartczak, Arthur Vigan, David Vokrouhlický, Emmanuel Jehin, E. Podlewska-Gaca, Toni Santana-Ros, Frédéric Vachier, M. Pajuelo, Paolo Tanga, S. Benseguane, Romain Fétick, Christophe Dumas, Grzegorz Dudziński, Mirel Birlan, Agnieszka Kryszczyńska, S. Fauvaud, Anna Marciniak, Benoit Carry, J. Berthier, Michael Marsset, Institute of Astronomy [Prague], Charles University [Prague] (CU), Search for Extraterrestrial Intelligence Institute (SETI), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Tampere University of Technology [Tampere] (TUT), Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, SETI Institute, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire du Bois de Bardon, Astronomical Institute of Romanian Academy, Romanian Academy, Thirty Meter Telescope Observatory, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP), Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Czech Science Foundation, Charles University (Czech Republic), National Science Foundation (US), National Aeronautics and Space Administration (US), Generalitat Valenciana, Ministerio de Ciencia, Innovación y Universidades (España), Fédération Wallonie-Bruxelles, and Belgian Science Policy Office
Subjects: 010504 meteorology & atmospheric sciences, fundamental parameters [Planets and satellites], Library science, FOS: Physical sciences, Astrophysics, 01 natural sciences, methods: numerical, Física Aplicada, 0103 physical sciences, Celestial mechanics, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], numerical [Methods], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Minor planets, Astronomy and Astrophysics, Astrometry, celestial mechanics, asteroids: individual: (216) Kleopatra, individual: (216) Kleopatra [Asteroids], Space and Planetary Science, individual: (216) Kleopatra [Minor planets, asteroids], minor planets, astrometry, TRAPPIST, Christian ministry, Earth and Planetary Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: [Aims] To interpret adaptive-optics observations of (216) Kleopatra, we need to describe an evolution of multiple moons orbiting an extremely irregular body and include their mutual interactions. Such orbits are generally non-Keplerian and orbital elements are not constants. [Methods] Consequently, we used a modified N-body integrator, which was significantly extended to include the multipole expansion of the gravitational field up to the order ℓ = 10. Its convergence was verified against the 'brute-force' algorithm. We computed the coefficients Cℓ m, Sℓ m for Kleopatra's shape, assuming a constant bulk density. For Solar System applications, it was also necessary to implement a variable distance and geometry of observations. Our χ2 metric then accounts for the absolute astrometry, the relative astrometry (second moon with respect to the first), angular velocities, and silhouettes, constraining the pole orientation. This allowed us to derive the orbital elements of Kleopatra's two moons. [Results] Using both archival astrometric data and new VLT/SPHERE observations (ESO LP 199.C-0074), we were able to identify the true periods of the moons, P1 = (1.822359 ± 0.004156) d, P2 = (2.745820 ± 0.004820) d. They orbit very close to the 3:2 mean-motion resonance, but their osculating eccentricities are too small compared to other perturbations (multipole, mutual), meaning that regular librations of the critical argument are not present. The resulting mass of Kleopatra, m1 = (1.49 ± 0.16) × 10-12 M· or 2.97 × 1018 kg, is significantly lower than previously thought. An implication explained in the accompanying paper is that (216) Kleopatra is a critically rotating body., Broz, M. et al., This work has been supported by the Czech Science Foundation through grant 21-11058S (M. Brož, D. Vokrouhlický), 20-08218S (J. Hanuš, J. Ďurech), and by the Charles University Research program No. UNCE/SCI/023. This material is partially based upon work supported by the National Science Foundation under Grant No. 1743015. P.V., A.D., M.F. and B.C. were supported by CNRS/INSU/PNP. M.M. was supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0849 issued through the Planetary Astronomy Program. The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liège, and performed in collaboration with Cadi Ayyad University of Marrakesh. E. Jehin is a FNRS Senior Research Associate.
Published: 2021

4. Magnetic reconnection leading to a mini-flare and a twisted jet observed with IRIS

Author: Joshi, Reetika, Schmieder, Brigitte, Chandra, Ramesh, Heinzel, Petr, Aulanier, Guillaume, Bommier, Véronique, Tomin, James, Vilmer, Nicole, Bommier, Véronique, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and European Physical Society (EPS)
Subjects: [PHYS.ASTR.SR] Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2021

5. AIDA DART asteroid deflection test: Planetary defense and science objectives

Author: Eugene G. Fahnestock, Olivier S. Barnouin, Lance A. M. Benner, Cristina A. Thomas, Justin A. Atchison, Emma S.G. Rainey, Carolyn M. Ernst, Petr Pravec, Nancy L. Chabot, Andrew S. Rivkin, Angela Stickle, A. F. Cheng, Michael Kueppers, Derek C. Richardson, Patrick Michel, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Operations Department (ESAC), European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), Ondřejov Observatory of the Prague Astronomical Institute, and Czech Academy of Sciences [Prague] (CAS)
Subjects: Orbital speed, 010504 meteorology & atmospheric sciences, 01 natural sciences, law.invention, Telescope, Impact crater, Deflection (engineering), law, 0103 physical sciences, Aerospace engineering, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, computer.programming_language, [PHYS]Physics [physics], Dart, business.industry, Rendezvous, Astronomy and Astrophysics, Orbital period, Space and Planetary Science, Asteroid, Environmental science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, computer
Abstract: The Asteroid Impact & Deflection Assessment (AIDA) mission is an international cooperation between NASA and ESA. NASA plans to provide the Double Asteroid Redirection Test (DART) mission which will perform a kinetic impactor experiment to demonstrate asteroid impact hazard mitigation. ESA proposes to provide the Hera mission which will rendezvous with the target to monitor the deflection, perform detailed characterizations, and measure the DART impact outcomes and momentum transfer efficiency. The primary goals of AIDA are (i) to demonstrate the kinetic impact technique on a potentially hazardous near-Earth asteroid and (ii) to measure and characterize the deflection caused by the impact. The AIDA target will be the binary asteroid (65803) Didymos, which is of spectral type Sq, with the deflection experiment to occur in October, 2022. The DART impact on the secondary member of the binary at ∼6 km/s changes the orbital speed and the binary orbit period, which can be measured by Earth-based observatories with telescope apertures as small as 1 m. The DART impact will in addition alter the orbital and rotational states of the Didymos binary, leading to excitation of eccentricity and libration that, if measured by Hera, can constrain internal structure of the target asteroid. Measurements of the DART crater diameter and morphology can constrain target properties like cohesion and porosity based on numerical simulations of the DART impact.
Published: 2018

6. European component of the AIDA mission to a binary asteroid Characterization and interpretation of the impact of the DART mission

Author: Ian Carnelli, Patrick Michel, Valérie Ciarletti, Stephen R. Schwartz, Özgür Karatekin, Derek C. Richardson, Karim Mellab, Naomi Murdoch, Antti Näsilä, Karri Muinonen, Petr Pravec, Stephan Ulamec, Holger Sierks, Alain Herique, Mikael Granvik, Olivier S. Barnouin, Erik Asphaug, Antti Kestilä, Antti Penttilä, Michael Kueppers, Tuomas Tikka, Kleomenis Tsiganis, Tomas Kohout, Adriano Campo Bagatin, Andrew S. Rivkin, Paolo Tortora, Andy F. Cheng, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Agence Spatiale Européenne (ESA), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), European Space Research and Technology Centre (ESTEC), Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Aalto University, Institute of Geology of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Finnish Geospatial Research Institute (FGI), VTT Technical Research Centre of Finland (VTT), Reaktor Space Lab, Dipartimento di Ingegneria Industriale [Forli], Università di Bologna [Bologna] (UNIBO), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Ondřejov Observatory of the Prague Astronomical Institute, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Aristotle University of Thessaloniki, Deutsches Zentrum für Luft- und Raumfahrt [Köln] (DLR), Royal Observatory of Belgium [Brussels], Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Institute of Geology of the Czech Academy of Sciences (GLI / CAS), Czech Academy of Sciences [Prague] (CAS), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), PLANETO - LATMOS, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Royal Observatory of Belgium [Brussels] (ROB), Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astronomía y Astrofísica, Michel, Patrick, Kueppers, Michael, Sierks, Holger, Carnelli, Ian, Cheng, Andy F., Mellab, Karim, Granvik, Mikael, Kestilä, Antti, Kohout, Toma, Muinonen, Karri, Näsilä, Antti, Penttila, Antti, Tikka, Tuoma, Tortora, Paolo, Ciarletti, Valérie, Hérique, Alain, Murdoch, Naomi, Asphaug, Erik, Rivkin, Andy, Barnouin, Olivier, Bagatin, Adriano Campo, Pravec, Petr, Richardson, Derek C., Schwartz, Stephen R., Tsiganis, Kleomeni, Ulamec, Stephan, Karatekin, Ozgür, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Atmospheric Science, Solar System, 010504 meteorology & atmospheric sciences, Computer science, ta1171, Aerospace Engineering, Binary number, 01 natural sciences, Mining, Near-Earth asteroid, Impact crater, Autre, Asteroid impact hazards, Física Aplicada, 0103 physical sciences, Binary asteroid, Aerospace engineering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, computer.programming_language, Dart, ta214, Near-Earth object, ta115, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Astronomy and Astrophysics, HERA, OtaNano, Near-Earth asteroids, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Kinetic impactor, Asteroid impact hazard, Asteroid resoureces utilization, Geophysics, 13. Climate action, Space and Planetary Science, Asteroid, Near-Erath asteroids, General Earth and Planetary Sciences, Planetary defense, Asteroid resources utilization, business, computer
Abstract: The European component of the joint ESA-NASA Asteroid Impact & Deflection Assessment (AIDA) mission has been redesigned from the original version called Asteroid Impact Mission (AIM), and is now called Hera. The main objectives of AIDA are twofold: (1) to perform an asteroid deflection test by means of a kinetic impactor under detailed study at NASA (called DART, for Double Asteroid Redirection Test); and (2) to investigate with Hera the changes in geophysical and dynamical properties of the target binary asteroid after the DART impact. This joint mission will allow extrapolating the results of the kinetic impact to other asteroids and therefore fully validate such asteroid deflection techniques. Hera leverages technology and payload pre-developments of the previous AIM, and focuses on key measurements to validate impact models such as the detailed characterisation of the impact crater. As such, AIDA will be the first documented deflection experiment and binary asteroid investigation. In particular, it will be the first mission to investigate a binary asteroid, and return new scientific knowledge with important implications for our understanding of asteroid formation and solar system history. Hera will investigate the smallest asteroid visited so far therefore providing a unique opportunity to shed light on the role cohesion and Van der Waals forces may play in the formation and resulting internal structure of such small bodies. P.M. acknowledges support from ESA. P.T. acknowledges support from ESA, through contract No. 4000117778/16/F/MOS Radio Science Investigation with AIM, for the assessment of the RSE capabilities. T.K. acknowledges support from the Academy of Finland project No. 285432. Institute of Geology, the Czech Academy of Sciences is supported by the Ministry of Education, Youth and Sports project No. RVO67985831. K.M. and A.P. acknowledge support from the ERC Advanced Grant No. 320773 (SAEMPL). P.P. was supported by the Grant Agency of the Czech Republic, Grant 17-00774S.
Published: 2017

7. Assessing possible mutual orbit period change by shape deformation of Didymos after a kinetic impact in the NASA-led Double Asteroid Redirection Test

Author: Shantanu P. Naidu, Masatoshi Hirabayashi, Derek C. Richardson, Angela Stickle, Andrew F. Cheng, Steven R. Chesley, Stephen R. Schwartz, Lance A. M. Benner, Daniel J. Scheeres, Patrick Michel, Petr Pravec, Martin Jutzi, E. Fahnestock, Andrew S. Rivkin, Yang Yu, A. B. Davis, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Flight Dynamics and Control (University of Michigan), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Shanghai Jiao Tong University [Shanghai], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Aerospace Engineering, Deformation (meteorology), Kinetic energy, 01 natural sciences, 0103 physical sciences, Ejecta, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, Work (physics), Astronomy and Astrophysics, Mechanics, Orbital period, 620 Engineering, Geophysics, Deflection (physics), Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], Physics::Space Physics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Spin (aerodynamics)
Abstract: The Asteroid Impact & Deflection Assessment (AIDA) targets binary near-Earth asteroid (65803) Didymos. As part of this mission, the NASA-led Double Asteroid Redirection Test (DART) will make a kinetic impactor collide with the smaller secondary of Didymos to test kinetic impact asteroid deflection technology, while the ESA-led Hera mission will evaluate the efficiency of the deflection by conducting detailed on-site observations. Research has shown that the larger primary of Didymos is spinning close to its critical spin, and the DART-impact-driven ejecta would give kinetic energy to the primary. It has been hypothesized that such an energy input might cause structural deformation of the primary, affecting the mutual orbit period, a critical parameter for assessing the kinetic impact deflection by the DART impactor. A key issue in the previous work was that the secondary was assumed to be spherical, which may not be realistic. Here, we use a second-order inertia-integral mutual dynamics model to analyze the effects of the shapes of the primary and the secondary on the mutual orbit period change of the system. We first compare the second-order model with three mutual dynamics models, including a high-order inertia-integral model that takes into account the detailed shapes of Didymos. The comparison tests show that the second-order model may have an error of ∼ 10 % for computing the mutual orbit period change, compared to the high-order model. We next use the second-order model to analyze how the original shape and shape deformation change the mutual orbit period. The results show that when the secondary is elongated, the mutual orbit period becomes short. Also, shape deformation of the secondary further changes the mutual orbit period. A better understanding of this mechanism allows for detailed assessment of DART’s kinetic impact deflection capability for Didymos.
Published: 2019
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8. Physical and Chemical Properties of Meteoroids

Author: Jiří Borovicka, Jean-Sébastien Macke, Campbell-Brown, Margaret D., Anny Chantal Levasseur-Regourd, Rietmeijer, Frans J. M., Tomáš Kohout, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Specola Vaticana/Vatican Observatory, University of Western Ontario (UWO), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), The University of New Mexico [Albuquerque], University of Helsinki, Galina Ryabova, David Asher and Margaret Campbell-Brown (eds), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, and Cardon, Catherine
Subjects: comet, asteroid, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], meteoroid composition, meteor, meteoroid element abundances, micrometeorite, interplanetary dust, meteoroid structure, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], meteoroid strength, meteorite, ComputingMilieux_MISCELLANEOUS
Abstract: International audience; The chapter provides a comprehensive and up to date review of physical properties (structure, strength, porosity etc.) and chemical composition of small solar system bodies with sizes ranging from several micrometers to several meters. Experts from different fields of research, using different methods, joined their efforts to present and compare results of laboratory investigation of meteorites, interplanetary dust particles (IDPs), and micrometeorites, studies of cometary and asteroidal dust by remote sensing, in-situ investigation or sample-return missions, and properties of meteoroids derived from observations of meteors. Meteors sample the whole population of meteoroids in the vicinity of the Earth and provide data of their orbits. The best currently available methods and models of inferring physical properties of meteoroids from their behavior during the atmospheric entry, in particular fragmentation, are discussed. Chemical compositions are extracted from meteor spectra. Perfectly designed figures and tables convey the information clearly and concisely to the reader. The data are relevant for understanding other solar system objects, especially comets and asteroids.
Published: 2019

9. Ultraviolet Spectropolarimetry as a Tool for Understanding the Diversity of Exoplanetary Atmospheres. Astro2020 Science White Paper

Author: Fossati, L., Rossi, Loïc, Stam, D., Garcia Muñoz, A., Berzosa-Molina, J., Marcos-Arenal, P., Caballero, J., Cabrera, J., Chiavassa, A., Désert, J.-M., Godolt, M., Grenfell, L., Haswell, C., Kabath, P., Kislyakova, K., Lanza, A., Lecavelier, A., Lendl, M., Pallé, E., Rauer, H., Rugheimer, S., Vidotto, A., Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), SRON Netherlands Institute for Space Research (SRON), Institut für Chemie [TUB Berlin], Technische Universität Berlin (TU), Technische Universiteit Delft (TU Delft), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Instituto Nacional de Técnica Aeroespacial (INTA), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Zentrum für Astronomie und Astrophysik [Berlin] (ZAA), The Open University [Milton Keynes] (OU), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), University of Vienna [Vienna], INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), DLR Institut für Planetenforschung, University of Oxford [Oxford], and Trinity College Dublin
Subjects: [SDU]Sciences of the Universe [physics], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics
Abstract: The polarization state of starlight reflected by a planetary atmosphere uniquely reveals coverage, particle size, and composition of aerosols as well as changing cloud patterns. It is not possible to obtain a comparable level of detailed from flux-only observations. Furthermore, polarization observations can probe the atmosphere of planets independently of the orbital geometry (i.e., transiting and non-transiting planets). We show that a high-resolution spectropolarimeter with a broad wavelength coverage, particularly if attached to a large space telescope, would enable simultaneous study of the polarimetric exoplanet properties of the continuum and to look for and characterize the polarimetric signal due to scattering from single molecules.
Published: 2019

10. CASTAway: An asteroid main belt tour and survey

Author: Henning Haack, Nicolas Thomas, Joan Pau Sánchez, J. de León, Andreas Nathues, Francesca E. DeMeo, Aurelie Guilbert-Lepoutre, A. Gibbings, Ian Thomas, Ákos Kereszturi, Fraser Clarke, Neil Bowles, Tristram Warren, C. M. Marriner, J. Leif Jorgensen, Matthias Tecza, V. Da Deppo, Naomi Murdoch, Alena Probst, Paul Eccleston, Andrew S. Rivkin, Ian Tosh, Sonia Fornasier, Thomas Andert, P. Pravec, K. L. Donaldson Hanna, Jessica A. Arnold, Mikael Granvik, Kjartan M. Kinch, Enzo Pascale, Benoit Carry, Ann Carine Vandaele, Colin Snodgrass, Giampiero Naletto, John K. Davies, Benjamin T. Greenhagen, Rhian H. Jones, Katherine H. Joy, Simon F. Green, Jessica Agarwal, Javier Licandro, J.M. Barnes, Laurent Jorda, Manish R. Patel, S. B. Calcutt, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Department of Mechanical and Aerospace Engineering [Glasgow], University of Strathclyde, Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Institut für Raumfahrttechnik, Universität der Bundeswehr München [Neubiberg] = Bundeswehr University, Laboratoire des Mécanismes et Transfert en Géologie (LMTG), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), FIME, Universidad Autonoma de Nuevo leon, Universidad Autonoma de Madrid (UAM), Institut universitaire des systèmes thermiques industriels (IUSTI), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), CNR Institute for Photonics and Nanotechnologies (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Collegium Budapest (Institute for Advanced Study) (CB), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (ASCR), Vetco Gray (VG), Vetco Gray, Cardiff University, Instituto de Astrofisica de Canarias (IAC), University of Oxford [Oxford], Department of Physics, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Universität der Bundeswehr München [Neubiberg]
Subjects: [SPI.OTHER]Engineering Sciences [physics]/Other, Atmospheric Science, Solar System, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], CERES, 7. Clean energy, 01 natural sciences, Star tracker, law.invention, Astrobiology, MAGNITUDE, Autre, law, P/2010 A2, SPACE-TELESCOPE, Survey, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), SPECTROSCOPY, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Remote sensing, Main Asteroid Belt, survey, flyby, mapping, remote sensing, Geophysics, Mapping, Asteroid, Asteroid belt, ROSETTA, Geology, SURFACE, Flyby, Aerospace Engineering, Space and Planetary Science, FOS: Physical sciences, Context (language use), Telescope, SOLAR-SYSTEM, 0103 physical sciences, 0105 earth and related environmental sciences, 21 LUTETIA, Spacecraft, business.industry, Payload, ICE, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, 13. Climate action, General Earth and Planetary Sciences, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: CASTAway is a mission concept to explore our Solar System's main asteroid belt. Asteroids and comets provide a window into the formation and evolution of our Solar System and the composition of these objects can be inferred from space-based remote sensing using spectroscopic techniques. Variations in composition across the asteroid populations provide a tracer for the dynamical evolution of the Solar System. The mission combines a long-range (point source) telescopic survey of over 10,000 objects, targeted close encounters with 10 to 20 asteroids and serendipitous searches to constrain the distribution of smaller (e.g. 10 m) size objects into a single concept. With a carefully targeted trajectory that loops through the asteroid belt, CASTAway would provide a comprehensive survey of the main belt at multiple scales. The scientific payload comprises a 50 cm diameter telescope that includes an integrated low-resolution (R = 30 to 100) spectrometer and visible context imager, a thermal (e.g. 6 to 16 microns) imager for use during the flybys, and modified star tracker cameras to detect small (approx. 10 m) asteroids. The CASTAway spacecraft and payload have high levels of technology readiness and are designed to fit within the programmatic and cost caps for a European Space Agency medium class mission, whilst delivering a significant increase in knowledge of our Solar System., 40 pages, accepted by Advances in Space Research October 2017
Published: 2018

11. Physical modeling of triple near-Earth Asteroid (153591) 2001 SN263 from radar and optical light curve observations

Author: Štefan Gajdoš, J. T. Pollock, Tracy M. Becker, Michael D. Hicks, Franck Marchis, N. M. Gaftonyuk, Adrian Galad, Yurij N. Krugly, Patrick A. Taylor, Jozef Vilagi, Ellen S. Howell, Brian D. Warner, Petr Pravec, Michael C. Nolan, Frederic Vachier, Igor Molotov, Leonard Kornoš, Christopher Magri, Julian Oey, A. Carbognani, David Higgins, University of Central Florida [Orlando] (UCF), Arecibo Observatory, National Astronomy and Ionosphere Center (NAIC), Cornell University [New York], University of Maine, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Leura Observatory, Hunters Hill Observatory, Modra Observatory, Comenius University in Bratislava, Crimean Astrophysical Observatory (CrAO), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), Keldysh Institute of Applied Mathematics, Russian Academy of Sciences [Moscow] (RAS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVDA), Center for Solar System Studies (CS3), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Carl Sagan Center, SETI Institute, Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, Near-Earth objects, 01 natural sciences, rotation, Photometry, 0103 physical sciences, Arecibo Observatory, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Near-Earth object, Asteroid, Ecliptic, Astronomy, Astronomy and Astrophysics, Light curve, Orbital period, Satellites of asteroids, Asteroids, Tidal locking, Radar observations, [SDU]Sciences of the Universe [physics], Asteroids, rotation, Space and Planetary Science
Abstract: We report radar observations (2380-MHz, 13-cm) by the Arecibo Observatory and optical light curves observed from eight different observatories and collected at the Ondřejov Observatory of the triple near-Earth asteroid system (153591) 2001 SN 263 . The radar observations were obtained over the course of ten nights spanning February 12–26, 2008 and the light curve observations were made throughout January 12 - March 31, 2008. Both data sets include observations during the object’s close approach of 0.06558 AU on February 20th, 2008. The delay-Doppler images revealed the asteroid to be comprised of three components, making it the first known triple near-Earth asteroid. Only one other object, (136617) 1994 CC is a confirmed triple near-Earth asteroid. We present physical models of the three components of the asteroid system. We constrain the primary’s pole direction to an ecliptic longitude and latitude of ( 309 ° , - 80 ° ) ± 15 ° . We find that the primary rotates with a period 3.4256 ± 0.0002 h and that the larger satellite has a rotation period of 13.43 ± 0.01 h , considerably shorter than its orbital period of approximately 6 days. We find that the rotation period of the smaller satellite is consistent with a tidally locked state and therefore rotates with a period of 0.686 ± 0.002 days (Fang et al. [2011]. Astron. J. 141, 154–168). The primary, the larger satellite, and the smaller satellite have equivalent diameters of 2.5 ± 0.3 km , 0.77 ± 0.12 km , 0.43 ± 0.14 km and densities of 1.1 ± 0.2 g / cm 3 , 1.0 ± 0.4 g / cm 3 , 2.3 ± 1.3 g / cm 3 , respectively.
Published: 2015
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12. The young Datura asteroid family

Author: Vokrouhlický, D., Pravec, P., Ďurech, J., Bolin, B., Jedicke, R., Kušnirák, P., Galad, A., Hornoch, K., Kryszczyńska, A., Colas, François, Moskovitz, N., Thirouin, A., Nesvorny, D., Institute of Astronomy, Charles University [Prague] (CU), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Astronomical Institute of Charles University, Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2017

13. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author: Valerio Nascimbeni, J. Lecacheux, Toni Santana-Ros, Agustín Sánchez-Lavega, Pablo Santos-Sanz, L. Nerli, D. T. Koseoglu, Frédéric Vachier, V. Peris, Przemyslaw Bartczak, R. Komžík, Eda Sonbas, Cs. Kiss, Gábor Marton, C. Ries, Yavuz Güney, Marcelo Assafin, Martina Maestripieri, Josselin Desmars, T. G. Mueller, Osman Demircan, O. Erece, V. Granata, A. R. Gomes-Júnior, Francesco Marzari, Ulrich Hopp, Cahit Yeşilyaprak, N. Paschalis, A. Campo Bagatin, B. Gaehrken, Paolo Bacci, V. Tsamis, O. Satir, F. Martinelli, F. L. Rommel, Santiago Pérez-Hoyos, F. Ciabattari, R. Iglesias-Marzoa, Stefano Mottola, Ricardo Hueso, Julio Camargo, Herman Mikuz, Françoise Roques, Mohammad Shameoni Niaei, Mauro Bachini, Vassilis Charmandaris, Jose Luis Ortiz, A. Takácsné Farkas, András Pál, A. Carbognani, L. Tzouganatos, Giuseppe Leto, Aleksandar Cikota, G. Benedetti-Rossi, Roberto Vieira-Martins, Nicolás Morales, José M. Madiedo, Bruno Sicardy, Róbert Szakáts, B. E. Morgado, Theodor Pribulla, Estela Fernández-Valenzuela, M. Butkiewicz-Bąk, Afşar Kabaş, Alvaro Alvarez-Candal, Giacomo Succi, Jérôme Berthier, J. Alikakos, Ç. Püsküllü, Kamil Hornoch, W. Beisker, E. Meza, Stefan Cikota, T. Ozisik, E. Varga-Verebélyi, J. M. Christille, J. C. Guirado, Grzegorz Dudziński, L. Mazzei, J. M. Ohlert, Rene Duffard, Raoul Behrend, S. Kalkan, A. Marciniak, N. Karaman, S. Hellmich, Kosmas Gazeas, Victor Ali-Lagoa, Ozan Ünsalan, Felipe Braga-Ribas, François Colas, Petr Pravec, Diane Berard, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astronomía y Astrofísica, ITA, USA, GBR, FRA, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatorio Nacional [Rio de Janeiro], Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatório Nacional/MCT, Ludwig-Maximilians-Universität München (LMU), Dipartimento di Fisica, Università degli Studi di Padova = University of Padua (Unipd), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Centro Astronomico di Libbiano, Associazione Astrofili Alta Valdera, Istituto di Informatica e Telematica (IIT-CNR), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), DLR Institute of Planetary Research, German Aerospace Center (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Physik-Institut, Universität Zürich [Zürich] = University of Zurich (UZH), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), International Occultation Timing Association European Section (IOTA ES), International Occultation Timing Association European Section, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), IESL, Osserv Astrofis Catania, Ist Nazl Astrofis, TKK Helsinki University of Technology (TKK), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Department of Astrophysics, Astronomy and Mechanics Panepistimiopolis (DAAMP), National and Kapodistrian University of Athens (NKUA), Astronomical Union of Sparta [Sparta], University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Departamento de Fı'sica Aplicada I, Escuela Tecnica Superior de Ingenieria Bilbao, Observatorio Astronomico de Valencia, Universitat de València (UV), Ondokuz Mayıs Üniversitesi, European Commission, European Research Council, Hungarian Academy of Sciences, Generalitat Valenciana, Junta de Andalucía, Ministerio de Economía, Industria y Competitividad (España), Universita degli Studi di Padova, Consiglio Nazionale delle Ricerche [Roma] (CNR), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), University of Geneva [Switzerland], University of the Basque Country [Bizkaia] (UPV/EHU), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Czech Academy of Sciences [Prague] (ASCR), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Zürich [Zürich] (UZH), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidade Federal do Rio de Janeiro [Rio de Janeiro] (UFRJ), Laboratoire d’Électrotechnique et d’Électronique de Puissance - EA 2697 (L2EP), Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille-Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Athens [Greece] (UOA), and Universitat de València (UV)-Observatorio Astronomico de Valencia
Subjects: 010504 meteorology & atmospheric sciences, European community, Trans Neptunian Object, Dwarf planet, Haumea, FOS: Physical sciences, Library science, shape, 01 natural sciences, size, dwarf planet, Neptune, Física Aplicada, 0103 physical sciences, media_common.cataloged_instance, European union, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], density, 2003 EL61, Kuiper-belt, photometric-observations, collisional family, object, bodies, albedo, satellites, Uranus, Dwarf planets, Multidisciplinary, European research, Asteroid, Trans-Neptunian, Astronomy, Stellar occultation, Moons of Haumea, stellar occultation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ring, Astrophysics - Earth and Planetary Astrophysics
Abstract: Ortiz, José Luis et. al., Haumea-one of the four known trans-Neptunian dwarf planets- is a very elongated and rapidly rotating body1-3. In contrast to other dwarf planets4-6, its size, shape, albedo and density are not well constrained. The Centaur Chariklo was the first body other than a giant planet known to have a ring system7, and the Centaur Chiron was later found to possess something similar to Chariklo's rings8,9. Here we report observations from multiple Earth-based observatories of Haumea passing in front of a distant star (a multichord stellar occultation). Secondary events observed around the main body of Haumea are consistent with the presence of a ring with an opacity of 0.5, width of 70 kilometres and radius of about 2,287 kilometres. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. The radius of the ring places it close to the 3:1 mean-motion resonance with Haumea's spin period-that is, Haumea rotates three times on its axis in the time that a ring particle completes one revolution. The occultation by the main body provides an instantaneous elliptical projected shape with axes of about 1,704 kilometres and 1,138 kilometres. Combined with rotational light curves, the occultation constrains the three-dimensional orientation of Haumea and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 kilometres, larger than previously thought, implying an upper limit for its density of 1,885 kilograms per cubic metre and a geometric albedo of 0.51, both smaller than previous estimates1,10,11. In addition, this estimate of the density of Haumea is closer to that of Pluto than are previous estimates, in line with expectations. No global nitrogen- or methane-dominated atmosphere was detected.© 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved., J.L.O. acknowledges funding from Spanish and Andalusian grants MINECO AYA-2014-56637-C2-1-P and J. A. 2012-FQM1776 as well as FEDER funds. Part of the research leading to these results received funding from the European Union's Horizon 2020 Research and Innovation Programme, under grant agreement no. 687378. B.S. acknowledges support from the French grants 'Beyond Neptune' ANR-08-BLAN-0177 and 'Beyond Neptune II' ANR-11-1S56-0002. Part of the research leading to these results has received funding from the European Research Council under the European Community's H2020 (2014-2020/ERG grant agreement no. 669416 'Lucky Star'). A.P. and R.S. have been supported by the grant LP2012-31 of the Hungarian Academy of Sciences. All of the Hungarian contributors acknowledge the partial support from K-125015 grant of the National Research, Development and Innovation Office (NKFIH). G.B.-R., F.B.-R., F.L.R., R.V.-M., J.I.B.C., M.A., A.R.G.-J. and B.E.M. acknowledge support from CAPES, CNPq and FAPERJ. J.C.G. acknowledges funding from AYA2015-63939-C2-2-P and from the Generalitat Valenciana PROMETEOII/2014/057. K.H. and P.P. were supported by the project RVO:67985815. The Astronomical Observatory of the Autonomous Region of the Aosta Valley acknowledges a Shoemaker NEO Grant 2013 from The Planetary Society. We acknowledge funds from a 2016 'Research and Education' grant from Fondazione CRT. We also acknowledge the Slovakian project ITMS no. 26220120029.
Published: 2017

14. Binary asteroid population. 3. Secondary rotations and elongations

Author: Jozef Vilagi, Stefano Mottola, Robert D. Stephens, Jean Lecacheux, R. Inasaridze, Dirk Terrell, Z. Krzeminski, B. Macomber, Shantanu P. Naidu, Peter Brown, Petr Pravec, Agnieszka Kryszczyńska, Daniel E. Reichart, Kamil Hornoch, R. Dyvig, R. Montaigut, John Gross, O. Kvaratskhelia, David Higgins, Vasilij Rumyantsev, Vladimir Benishek, J. Žižka, V. R. Ayvazian, Vishnu Reddy, F. Marchis, A. Leroy, J. Vrastil, Igor Molotov, Yu. N. Krugly, R. Durkee, Adrian Galad, Aaron P. LaCluyze, Štefan Gajdoš, Vasilij G. Chiorny, Walter R. Cooney, Julian Oey, S. Hellmich, M. Baek, N. Gaftonyuk, J. G. Ries, J. B. Haislip, Leonard Kornoš, Peter Kusnirak, Marek Husárik, François Colas, P. Scheirich, Joe Pollock, Donald P. Pray, G. Masi, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Physics Division [Oak Ridge], Oak Ridge National Laboratory [Oak Ridge] (ORNL), UT-Battelle, LLC-UT-Battelle, LLC, Sonoita Research Observatory, Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Skalnaté Pleso Observatory, Shed of Science Observatory, UND Department of Space Studies, University of North Dakota [Grand Forks] (UND), German Aerospace Center (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Kingsgrove Observatory, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), SETI Institute, Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, and HESAM Université (HESAM)-HESAM Université (HESAM)
Subjects: 010504 meteorology & atmospheric sciences, Fission, Population, Orbital eccentricity, Astrophysics, Rotation, Near-Earth objects, 01 natural sciences, rotation, Photometry, 0103 physical sciences, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], education.field_of_study, Near-Earth object, Astronomy, Astronomy and Astrophysics, dynamics, Asteroids, Astron, Space and Planetary Science, Asteroid, Tidal circularization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We collected data on rotations and elongations of 46 secondaries of binary and triple systems among near-Earth, Mars-crossing and small main belt asteroids. 24 were found or are strongly suspected to be synchronous (in 1:1 spin–orbit resonance), and the other 22, generally on more distant and/or eccentric orbits, were found or are suggested to have asynchronous rotations. For 18 of the synchronous secondaries, we constrained their librational angles, finding that their long axes pointed to within 20° of the primary on most epochs. The observed anti-correlation of secondary synchroneity with orbital eccentricity and the limited librational angles agree with the theories by Cuk and Nesvorný (Cuk, M., Nesvorný, D. [2010]. Icarus 207, 732–743) and Naidu and Margot (Naidu, S.P., Margot, J.-L. [2015]. Astron. J. 149, 80). A reason for the asynchronous secondaries being on wider orbits than synchronous ones may be longer tidal circularization time scales at larger semi-major axes. The asynchronous secondaries show relatively fast spins; their rotation periods are typically 10 h. An intriguing observation is a paucity of chaotic secondary rotations; with an exception of (35107) 1991 VH, the secondary rotations are single-periodic with no signs of chaotic rotation and their periods are constant on timescales from weeks to years. The secondary equatorial elongations show an upper limit of a 2 / b 2 ∼ 1.5 . The lack of synchronous secondaries with greater elongations appears consistent, considering uncertainties of the axis ratio estimates, with the theory by Cuk and Nesvorný that predicts large regions of chaotic rotation in the phase space for a 2 / b 2 ≳ 2 . Alternatively, secondaries may not form or stay very elongated in gravitational (tidal) field of the primary. It could be due to the secondary fission mechanism suggested by Jacobson and Scheeres (Jacobson, S.A., Scheeres, D.J. [2011]. Icarus 214, 161–178), as its efficiency is correlated with the secondary elongation. Sharma (Sharma, I. [2014]. Icarus 229, 278–294) found that rubble-pile satellites with a 2 / b 2 ≲ 1.5 are more stable to finite structural perturbations than more elongated ones. It appears that more elongated secondaries, if they originally formed in spin fission of parent asteroid, are less likely to survive intact and they more frequently fail or fission.
Published: 2016

15. Science case for the Asteroid Impact Mission (AIM): A component of the Asteroid Impact & Deflection Assessment (AIDA) mission

Author: Ian Carnelli, Patrick Michel, Michael Küppers, Jens Biele, Olivier S. Barnouin, Derek C. Richardson, Andres Galvez, P. Scheirich, Jürgen Blum, Stephen R. Schwartz, Yang Yu, Andrew F. Cheng, Marco Delbo, Simon F. Green, Kleomenis Tsiganis, Audrey Thirouin, A. Campo Bagatin, Pascal Rosenblatt, Lance A. M. Benner, Stephan Ulamec, Shantanu P. Naidu, Petr Pravec, Jean-Baptiste Vincent, Nicholas Moskovitz, Alain Herique, Valérie Ciarletti, Andrew S. Rivkin, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (ASCR), Technische Universität Braunschweig [Braunschweig], School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Royal Observatory of Belgium [Brussels], Aristotle University of Thessaloniki, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, German Aerospace Center (DLR), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne (ESA), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Lowell Observatory [Flagstaff], Universidad de Alicante, EUropean Space Agency (ESA), NASA, Agency of the Czech Republic, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astronomía y Astrofísica, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Czech Academy of Sciences [Prague] (CAS), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Royal Observatory of Belgium [Brussels] (ROB), PLANETO - LATMOS, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), and NASA-California Institute of Technology (CALTECH)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Aerospace Engineering, kinetic impactor, 01 natural sciences, Space exploration, Astrobiology, Asteroid impact hazards, Deflection (engineering), Física Aplicada, near-earth asteroids, 0103 physical sciences, Aerospace engineering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Near-Earth object, Binary asteroids, Spacecraft, business.industry, Rendezvous, Data interpretation, Astronomy and Astrophysics, Planetary defence, Near-Earth asteroids, Kinetic impactor, Nutzerzentrum für Weltraumexperimente (MUSC), Geophysics, Space and Planetary Science, Asteroid, Asteroid Impact hazards, General Earth and Planetary Sciences, Planetary defense, business, binary asteroids
Abstract: The Asteroid Impact & Deflection Assessment (AIDA) mission is a joint cooperation between European and US space agencies that consists of two separate and independent spacecraft that will be launched to a binary asteroid system, the near-Earth asteroid Didymos, to test the kinetic impactor technique to deflect an asteroid. The European Asteroid Impact Mission (AIM) is set to rendezvous with the asteroid system to fully characterize the smaller of the two binary components a few months prior to the impact by the US Double Asteroid Redirection Test (DART) spacecraft. AIM is a unique mission as it will be the first time that a spacecraft will investigate the surface, subsurface, and internal properties of a small binary near-Earth asteroid. In addition it will perform various important technology demonstrations that can serve other space missions. The knowledge obtained by this mission will have great implications for our understanding of the history of the Solar System. Having direct information on the surface and internal properties of small asteroids will allow us to understand how the various processes they undergo work and transform these small bodies as well as, for this particular case, how a binary system forms. Making these measurements from up close and comparing them with ground-based data from telescopes will also allow us to calibrate remote observations and improve our data interpretation of other systems. With DART, thanks to the characterization of the target by AIM, the mission will be the first fully documented impact experiment at asteroid scale, which will include the characterization of the target’s properties and the outcome of the impact. AIDA will thus offer a great opportunity to test and refine our understanding and models at the actual scale of an asteroid, and to check whether the current extrapolations of material strength from laboratory-scale targets to the scale of AIDA’s target are valid. Moreover, it will offer a first check of the validity of the kinetic impactor concept to deflect a small body and lead to improved efficiency for future kinetic impactor designs. This paper focuses on the science return of AIM, the current knowledge of its target from ground-based observations, and the instrumentation planned to get the necessary data. The authors acknowledge support from ESA and NASA. The work of P.P. and P.S. was supported by the Grant Agency of the Czech Republic, Grant 15-07193S.
Published: 2016

16. The tumbling spin state of (99942) Apophis

Author: K. M. Ivarsen, Joe Pollock, Michaël Gillon, Jean Manfroid, Daniel E. Reichart, Julian Oey, Cyrielle Opitom, Adrian Galad, David Vokrouhlický, Peter Kusnirak, Kamil Hornoch, Josef Ďurech, Emmanuel Jehin, P. Scheirich, J. Vrastil, Petr Pravec, François Colas, Aaron P. LaCluyze, Alan W. Harris, J. B. Haislip, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Astronomical Institute of Charles University, Charles University [Prague] (CU), Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Institute of Astronomy, European Southern Observatory (ESO), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Kingsgrove Observatory, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: Physics, [PHYS]Physics [physics], education.field_of_study, Angular momentum, 010504 meteorology & atmospheric sciences, Population, Astronomy, Astronomy and Astrophysics, Moment of inertia, Rotation, 01 natural sciences, Rotational energy, Space and Planetary Science, Asteroid, Excited state, 0103 physical sciences, Precession, Atomic physics, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: Our photometric observations of Asteroid (99942) Apophis from December 2012 to April 2013 revealed it to be in a state of non-principal axis rotation (tumbling). We constructed its spin and shape model and found that it is in a moderately excited Short Axis Mode (SAM) state with a ratio of the rotational kinetic energy to the basic spin state energy E / E 0 = 1.024 ± 0.013 . (All quoted uncertainties correspond to 3 σ .) The greatest and intermediate principal moments of inertia are nearly the same with I 2 / I 3 = 0.965 - 0.015 + 0.009 , but the smallest principal moment of inertia is substantially lower with I 1 / I 3 = 0.61 - 0.08 + 0.11 ; the asteroid’s dynamically equivalent ellipsoid is close to a prolate ellipsoid. The precession and rotation periods are P ϕ = 27.38 ± 0.07 h and P ψ = 263 ± 6 h , respectively; the strongest observed lightcurve amplitude for the SAM case is in the 2nd harmonic of P 1 = P ϕ - 1 - P ψ - 1 - 1 = 30.56 ± 0.01 h . The rotation is retrograde with the angular momentum vector’s ecliptic longitude and latitude of 250° and - 75 ° (the uncertainty area is approximately an ellipse with the major and minor semiaxes of 27° and 14 ° , respectively). An implication of the retrograde rotation is a somewhat increased probability of the Apophis’ impact in 2068, but it is still very small with the risk level on the Palermo Scale remaining well below zero. Apophis is a member of the population of slowly tumbling asteroids. Applying the theory of asteroid nutational damping by Breiter et al. (Breiter, S., Rozek, A., Vokrouhlický, D. [2012]. Mon. Not. R. Astron. Soc. 427, 755–769), we found that slowly tumbling asteroids predominate in the spin rate–size range where their estimated damping times are greater than about 0.2 Gyr. The appearance that the PA/NPA rotators transition line seems to follow a line of constant damping time may be because there are two or more asteroid spin evolution mechanisms in play, or the factor of μ Q (the elastic modulus times the quality factor) is not constant but it may decrease with decreasing asteroid size, which would oppose the trend due to decreasing collisional age or excitation time.
Published: 2014

17. Analysis of the rotation period of asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger - search for the YORP effect

Author: Franck Marchis, Brian D. Warner, V. Fuller, Yu. N. Krugly, David Polishook, Igor Molotov, Petr Pravec, Josef Ďurech, Matti Viikinkoski, O. A. Burkhonov, R. Ya. Inasaridze, B. Macomber, Walter R. Cooney, Sławomir Breiter, Robert D. Stephens, N. M. Gaftonyuk, David Vokrouhlický, Z. Vanderplate, Joe Pollock, Gy. M. Szabó, Julian Oey, Dirk Terrell, Frédéric Vachier, E. Litvinenko, I. Slyusarev, Vasilij G. Shevchenko, Krisztián Sárneczky, O. I. Kvaratshelia, John Gross, Mikko Kaasalainen, A. Baransky, Astronomical Institute of Charles University, Charles University [Prague], Astronomical Observatory, Taras Shevchenko National University of Kyiv, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań ( UAM ), Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Sonoita Research Observatory, Department of Physics and Astronomy, Appalachian State University, Crimean Astrophysical Observatory ( CrAO ), Abastumani Astrophysical Observatory, Ilia State University [ Tbilisi], Department of Mathematics [Tampere], Tampere University of Technology [Tampere] ( TUT ), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University ( KhNU ), The Central Pulkovo Astronomical Observatory, Russian Academy of Sciences [Moscow] ( RAS ), Astronomy Department [Berkeley], University of California [Berkeley], Carl Sagan Center, SETI Institute, Keldysh Institute of Applied Mathematics, Kingsgrove Observatory, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] ( EAPS ), Massachusetts Institute of Technology ( MIT ), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] ( ASCR ), Konkoly Observatory, Hungarian Academy of Sciences [Budapest], Goat Mountain Astronomical Research Station, Department of Experimental Physics, University of Szeged [Szeged], ELTE Gao-Lendulet Research Group, Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Palmer Divide Observatory, Charles University [Prague] (CU), Astronomical Observatory of Kiev, Adam Mickiewicz University in Poznań (UAM), Uzbekistan Academy of Sciences, Department of Physics and Astronomy [Boone], University of North Carolina System (UNC)-University of North Carolina System (UNC), Crimean Astrophysical Observatory (CrAO), Ilia State University [Tbilisi], Tampere University of Technology [Tampere] (TUT), V.N. Karazin Kharkiv National University (KhNU), Russian Academy of Sciences [Moscow] (RAS), Department of Astronomy [Berkeley], University of California-University of California, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Czech Academy of Sciences [Prague] (CAS), Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), ELTE Gothard Astrophysical Observatory, Eötvös Loránd University (ELTE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Rotation period, Physics, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astronomy and Astrophysics, Acceleration (differential geometry), Context (language use), Astrophysics, Rotation, Light curve, 01 natural sciences, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Photometry (optics), [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Space and Planetary Science, Asteroid, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: The original publication is available at www.aanda.org. Copyright ESO.; International audience; The spin state of small asteroids can change on a long timescale by the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect, the net torque that arises from anisotropically scattered sunlight and proper thermal radiation from an irregularly-shaped asteroid. The secular change in the rotation period caused by the YORP effect can be detected by analysis of asteroid photometric lightcurves. We analyzed photometric lightcurves of near-Earth asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger with the aim to detect possible deviations from the constant rotation caused by the YORP effect. We carried out new photometric observations of the three asteroids, combined the new lightcurves with archived data, and used the lightcurve inversion method to model the asteroid shape, pole direction, and rotation rate. The YORP effect was modeled as a linear change in the rotation rate in time d\omega /dt. Values of d\omega/ dt derived from observations were compared with the values predicted by theory. We derived physical models for all three asteroids. We had to model Eger as a nonconvex body because the convex model failed to fit the lightcurves observed at high phase angles. We probably detected the acceleration of the rotation rate of Eger d\omega / dt = (1.4 +/- 0.6) x 10^{-8} rad/d (3\sigma error), which corresponds to a decrease in the rotation period by 4.2 ms/yr. The photometry of Cerberus and Ra-Shalom was consistent with a constant-period model, and no secular change in the spin rate was detected. We could only constrain maximum values of |d\omega / dt| < 8 x 10^{-9} rad/d for Cerberus, and |d\omega / dt| < 3 x 10^{-8} rad/d for Ra-Shalom.
Published: 2012

18. Deducing Electron Properties From Hard X-Ray Observations

Author: Wojtek Hajdas, Anna Maria Massone, Jana Kašparová, Gordon D. Holman, John C. Brown, A. G. Emslie, Procheta Mallik, G. J. Hurford, E. J. Schmahl, Mark L. McConnell, Michele Piana, Eduard P. Kontar, E. Suarez-Garcia, Marco Prato, University of Glasgow, Paul Scherrer Institute (PSI), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Dipartimento di Matematica [Genova], and Universita degli studi di Genova
Subjects: Photon, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Electron, Radiation, 01 natural sciences, Sun flares, Sun X-rays, Sun acceleration, Sun energetic particles, Physics - Space Physics, Hard X-ray spectroscopy, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, imaging and imaging spectroscopy, Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar flare, Astronomy and Astrophysics, Photoelectric effect, Polarization (waves), Space Physics (physics.space-ph), Physics - Plasma Physics, Computational physics, Particle acceleration, Plasma Physics (physics.plasm-ph), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: X-radiation from energetic electrons is the prime diagnostic of flare-accelerated electrons. The observed X-ray flux (and polarization state) is fundamentally a convolution of the cross-section for the hard X-ray emission process(es) in question with the electron distribution function, which is in turn a function of energy, direction, spatial location and time. To address the problems of particle propagation and acceleration one needs to infer as much information as possible on this electron distribution function, through a deconvolution of this fundamental relationship. This review presents recent progress toward this goal using spectroscopic, imaging and polarization measurements, primarily from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). Previous conclusions regarding the energy, angular (pitch angle) and spatial distributions of energetic electrons in solar flares are critically reviewed. We discuss the role and the observational evidence of several radiation processes: free-free electron-ion, free-free electron-electron, free-bound electron-ion bremsstrahlung, photoelectric absorption and Compton back-scatter (albedo), using both spectroscopic and imaging techniques. This unprecedented quality of data allows for the first time inference of the angular distributions of the X-ray-emitting electrons using albedo, improved model-independent inference of electron energy spectra and emission measures of thermal plasma. Moreover, imaging spectroscopy has revealed hitherto unknown details of solar flare morphology and detailed spectroscopy of coronal, footpoint and extended sources in flaring regions. Additional attempts to measure hard X-ray polarization were not sufficient to put constraints on the degree of anisotropy of electrons, but point to the importance of obtaining good quality polarization data., This is an article for a monograph on the physics of solar flares, inspired by RHESSI observations. The individual articles are to appear in Space Science Reviews (2011); 10.1007/s11214-011-9804-x
Published: 2011

19. Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes

Author: Josef Hanus, Brad Timerson, Josef Ďurech, Frederick Pilcher, D. Dunham, Mikko Kaasalainen, Adrian Galad, Brian D. Warner, D. Herald, E. Frappa, John Talbot, Tsutomu Hayamizu, Faculty of Mathematics and Physics [Praha/Prague], Charles University [Prague], Department of Mathematics [Tampere], Tampere University of Technology [Tampere] ( TUT ), Occultation Section, Palmer Divide Observatory, FMFI Comenius University, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] ( ASCR ), Charles University [Prague] (CU), Tampere University of Technology [Tampere] (TUT), and Czech Academy of Sciences [Prague] (CAS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Inverse transform sampling, Astronomy, Astronomy and Astrophysics, Light curve, 01 natural sciences, Occultation, Asteroids, Silhouette, Photometry (optics), Photometry, Stars, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Occultations, 010303 astronomy & astrophysics, Geology, [ SDU ] Sciences of the Universe [physics], 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Asteroid sizes can be directly measured by observing occultations of stars by asteroids. When there are enough observations across the path of the shadow, the asteroid's projected silhouette can be reconstructed. Asteroid shape models derived from photometry by the lightcurve inversion method enable us to predict the orientation of an asteroid for the time of occultation. By scaling the shape model to fit the occultation chords, we can determine the asteroid size with a relative accuracy of typically ~ 10%. We combine shape and spin state models of 44 asteroids (14 of them are new or updated models) with the available occultation data to derive asteroid effective diameters. In many cases, occultations allow us to reject one of two possible pole solutions that were derived from photometry. We show that by combining results obtained from lightcurve inversion with occultation timings, we can obtain unique physical models of asteroids., 33 pages, 45 figures, 4 tables, accepted for publication in Icarus
Published: 2011

20. Spectroscopic study of comet Halley by the Vega 2 three-channel spectrometer

Author: V.S. Troshin, G. Moreels, T. Gogosheva, M. Vincent, K. Palazov, A. A. Krysko, J. Clairemidi, V. I. Moroz, V. A. Krasnopolsky, M. Gogoshev, J. L. Bertaux, J. E. Blamont, B. Valnicek, S. Sargoichev, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Observatory Stara Zagora, Université de Besançon, Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ondřejov Observatory of the Prague Astronomical Institute, and Czech Academy of Sciences [Prague] (CAS)
Subjects: Physics, Multidisciplinary, Interplanetary dust cloud, Spectrometer, Infrared, Halley's Comet, Comet, Analytical chemistry, Astronomy, Astronomical spectroscopy, Cosmochemistry, Cosmic dust, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: The three-channel spectrometer (TKS) aboard the Vega 2 spacecraft recorded infrared and visible spectra near the nucleus of comet Halley. Spectra in the range 0.95–1.9 µm at a distance of 300 km from the nucleus reveal the H2O 1.38-µm band and OH bands, the latter excited by dissociation of a parent molecule. Their production rates are 4 × 1029 and 1.7 × 1030 molecules s−1, respectively. The dust particle density is 0.35 g cm−3, typical of fluffy particles of interplanetary dust. Emissions of 10 species are observed in the range 275–715 nm at ∼4,000 km from the nucleus, and 6 of them are analysed in terms of production rates: QOH = 2×1030, QCH = 1029, = 6×1027, = 3×1027, QCN = 1027 and QNH = 2 × 1026, all in molecules s−1. The difference between the OH and H2O production rates is puzzling and needs further analysis. Ionic emissions, not discussed here, are prominent in the tailward part of the comet.
Published: 1986

21. Television observations of comet Halley from Vega spacecraft

Author: R. Z. Sagdeev, F. Szabó, G. A. Avanesov, P. Cruvellier, L. Szabó, K. Szegő, A. Abergel, A. Balazs, I. V. Barinov, J.-L. Bertaux, J. Blamont, M. Detaille, E. Demarelis, G. N. Dul'nev, G. Endröczy, M. Gardos, M. Kanyo, V. I. Kostenko, V. A. Krasikov, T. Nguyen-Trong, Z. Nyitrai, I. Reny, P. Rusznyak, V. A. Shamis, B. Smith, K. G. Sukhanov, S. Szalai, V. I. Tarnopolsky, I. Toth, G. Tsukanova, B. I. Valníček, L. Varhalmi, Yu. K. Zaiko, S. I. Zatsepin, Ya. L. Ziman, M. Zsenei, B. S. Zhukov, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Laboratoire d'Astronomie Spatiale (LAS), Centre National de la Recherche Scientifique (CNRS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Leningrad Institute of Fine Mechanics and Optics (ITMO), Ondřejov Observatory of the Prague Astronomical Institute, and Czech Academy of Sciences [Prague] (CAS)
Subjects: Physics, Multidisciplinary, Spacecraft, business.industry, Television system, Halley's Comet, Comet, Vega, Astronomy, Albedo, Spectral line, medicine.anatomical_structure, [SDU]Sciences of the Universe [physics], medicine, business, Nucleus
Abstract: International audience; The television system (TVS) aboard the spacecraft Vega 1 and Vega 2 observed comet Halley from 4 to 11 March 1986, and transmitted ∼1,500 images to Earth. The best images of the cometary nucleus were obtained from distances of 8,000–9,000 km. The nucleus is an irregular potato-shaped body, ∼14 × 7.5 × 7.5 km in size, which rotates with a period of 53±3 h. The surface is rather dark; the measured albedo is ∼0.04−0.01+0.02. Active emission of matter was observed on the sunlit side of the nucleus.
Published: 1986

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21 results on '"Ondřejov Observatory of the Prague Astronomical Institute"'

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19. Combining asteroid models derived by lightcurve inversion with asteroidal occultation silhouettes

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21. Television observations of comet Halley from Vega spacecraft

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21 results on '"Ondřejov Observatory of the Prague Astronomical Institute"'

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