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23 results on '"Institute of Physics [Graz]"'

1. Cometary Dust

Author: Anny-Chantal Levasseur-Regourd, Jessica Agarwal, Hervé Cottin, Cécile Engrand, George Flynn, Marco Fulle, Tamas Gombosi, Yves Langevin, Jérémie Lasue, Thurid Mannel, Sihane Merouane, Olivier Poch, Nicolas Thomas, Andrew Westphal, 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), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), State University of New York at Plattsburgh (SUNY Plattsburgh), State University of New York (SUNY), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), Institute of Physics [Graz], University of Graz, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), Physikalisches Institut [Bern], Universität Bern [Bern], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, PLANETO - 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Karl-Franzens-Universität [Graz, Autriche], 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 Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Karl-Franzens-Universität Graz, Universität Bern [Bern] (UNIBE), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), and Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Aggregates, Jupiter-family comets, Astrophysics::Cosmology and Extragalactic Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, complex mixtures, Nucleus, Article, Organics, 0103 physical sciences, Rosetta, Comets, Astrophysics::Solar and Stellar Astrophysics, Coma, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, Astronomy and Astrophysics, Dust, 620 Engineering, Stardust, respiratory tract diseases, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Trail
Abstract: International audience; This review presents our understanding of cometary dust at the end of 2017. For decades, insight about the dust ejected by nuclei of comets had stemmed from remote observations from Earth or Earth’s orbit, and from flybys, including the samples of dust returned to Earth for laboratory studies by the Stardust return capsule. The long-duration Rosetta mission has recently provided a huge and unique amount of data, obtained using numerous instruments, including innovative dust instruments, over a wide range of distances from the Sun and from the nucleus. The diverse approaches available to study dust in comets, together with the related theoretical and experimental studies, provide evidence of the composition and physical properties of dust particles, e.g., the presence of a large fraction of carbon in macromolecules, and of aggregates on a wide range of scales. The results have opened vivid discussions on the variety of dust-release processes and on the diversity of dust properties in comets, as well as on the formation of cometary dust, and on its presence in the near-Earth interplanetary medium. These discussions stress the significance of future explorations as a way to decipher the formation and evolution of our Solar System.
Published: 2022
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2. Investigating Mercury's Environment with the Two-Spacecraft BepiColombo Mission

Author: Oleg Korablev, M. Fujimoto, Léa Griton, Cesare Grava, Masafumi Hirahara, Hirotsugu Kojima, S. Barabash, Wolfgang Baumjohann, A. Martindale, Chuanfei Dong, François Leblanc, Chris Carr, S. T. Lindsay, Yasumasa Kasaba, M. Kobayashi, Herbert Lichtenegger, Philippe-A. Bourdin, Karri Muinonen, J. S. Oliveira, Jan-Erik Wahlund, Ferdinand Plaschke, Christina Plainaki, S. M. P. McKenna-Lawlor, Dominique Delcourt, Eric Quémerais, Xianzhe Jia, Dusan Odstrcil, James A. Slavin, V. Mangano, M. G. Pelizzo, Benoit Langlais, Joe Zender, Emma J. Bunce, Ichiro Yoshikawa, Peter Wurz, Stavro Ivanovski, Stefano Massetti, George C. Ho, Y. Saito, Juhani Huovelin, Suzanne M. Imber, Sae Aizawa, Alessandro Mura, Jim M. Raines, Ayako Matsuoka, F. Sahraoui, Karl-Heinz Glassmeier, Pierre Henri, Rami Vainio, Matthew K. James, Rosemary M. Killen, Stefano Orsini, Shahab Fatemi, Tomas Karlsson, Monica Laurenza, Esa Kallio, Christoph Lhotka, Michiko Morooka, Johannes Benkhoff, David A. Rothery, Yasuhito Narita, Michel Moncuquet, Anna Milillo, Alexey A. Berezhnoy, Satoshi Yagitani, Adam Masters, F. Califano, Manuel Grande, Stefano Livi, Daniel Heyner, Emilia Kilpua, G. Murakami, Jan Deca, S. de la Fuente, R. Moissl, Bernard V. Jackson, Kanako Seki, N. André, M. Dósa, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Space Research Centre [Leicester], University of Leicester, Department of Space and Plasma Physics [Stockholm], KTH School of Electrical Engineering, Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), NASA Goddard Space Flight Center (GSFC), Space Technology Ireland Limited, Department of Climate and Space Sciences and Engineering (CLaSP), 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Sternberg Astronomical Institute [Moscow], Lomonosov Moscow State University (MSU), University of Pisa - Università di Pisa, University of Colorado [Boulder], European Space Astronomy Centre (ESAC), Princeton Plasma Physics Laboratory (PPPL), Princeton University, Department of Astrophysical Sciences [Princeton], Southwest Research Institute [San Antonio] (SwRI), Swedish Institute of Space Physics [Kiruna] (IRF), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), INAF - Osservatorio Astronomico di Trieste (OAT), University of California [San Diego] (UC San Diego), University of California (UC), Department of Electronics and Nanoengineering [Espoo], School of Electrical Engineering [Aalto Univ], Aalto University-Aalto University, Planetary Plasma and Atmospheric Research Center [Sendai] (PPARC), Tohoku University [Sendai], Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Blackett Laboratory, Imperial College London, Swedish Institute of Space Physics [Uppsala] (IRF), Institute of Physics [Graz], Karl-Franzens-Universität Graz, Centro de Investigação da Terra e do Espaço da UC (CITEUC), Universidade de Coimbra [Coimbra], CNR Institute for Photonics and Nanotechnologies (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Italian Space Agency, 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), Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Space Research Laboratory [Turku] (SRL), Department of Physics and Astronomy [Turku], University of Turku-University of Turku, Physics Institute [Bern], University of Bern, Department of Physics [Imperial College London], Institute of Mathematical and Physical Sciences [Aberystwyth], University of Wales, Institute for Space-Earth Environmental Research [Nagoya] (ISEE), Nagoya University, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Research Institute for Sustainable Humanosphere (RISH), Kyoto University, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), 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), Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Department of Complexity Science and Engineering [Tokyo], The University of Tokyo (UTokyo), European Space Agency (ESA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), University of California, University of Helsinki-University of Helsinki, 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), Karl-Franzens-Universität [Graz, Autriche], Consiglio Nazionale delle Ricerche [Roma] (CNR), Kyoto University [Kyoto], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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), The Royal Society, Science and Technology Facilities Council, INAF National Institute for Astrophysics, JAXA Institute of Space and Astronautical Science, European Space Research and Technology Centre, IRAP, Hungarian Academy of Sciences, Technical University of Braunschweig, Johns Hopkins Applied Physics Laboratory, University of Michigan, Ann Arbor, KTH Royal Institute of Technology, NASA Goddard Space Flight Center, Space Technology Ireland, Open University Milton Keynes, Austrian Academy of Sciences, Lomonosov Moscow State University, University of Pisa, University of Colorado Boulder, European Space Astronomy Centre, Princeton Plasma Physics Laboratory, Southwest Research Institute, Uppsala University, Université d'Orléans, Osservatorio Astronomico di Trieste, University of California San Diego, Department of Electronics and Nanoengineering, Tohoku University, University of Helsinki, Chiba Institute of Technology, Université de Nantes, Sorbonne Université, University of Graz, National Research Council of Italy, Agenzia Spaziale Italiana, The University of Tokyo, University of Turku, Aberystwyth University, Space Research Institute of the Russian Academy of Sciences, Université de Versailles Saint-Quentin-en-Yvelines, Kanazawa University, Aalto-yliopisto, and Aalto University
Subjects: 010504 meteorology & atmospheric sciences, Computer science, BepiColombo, chemistry.chemical_element, FOS: Physical sciences, Astronomy & Astrophysics, 01 natural sciences, Mercury’s environment, Fusion, plasma och rymdfysik, Interplanetary dust cloud, Astronomi, astrofysik och kosmologi, 0201 Astronomical and Space Sciences, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Exosphere, Magnetosphere, Aerospace engineering, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Scientific instrument, Earth and Planetary Astrophysics (astro-ph.EP), Spacecraft, business.industry, 520 Astronomy, Astronomy and Astrophysics, 620 Engineering, Fusion, Plasma and Space Physics, Mercury (element), Solar wind, Planetary science, chemistry, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Mercury's environment, Mercury’s environment · Magnetosphere · Exosphere · BepiColombo, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Earth and Planetary Astrophysics
Abstract: The ESA-JAXA BepiColombo mission will provide simultaneous measurements from two spacecraft, offering an unprecedented opportunity to investigate magnetospheric and exospheric dynamics at Mercury as well as their interactions with the solar wind, radiation, and interplanetary dust. Many scientific instruments onboard the two spacecraft will be completely, or partially devoted to study the near-space environment of Mercury as well as the complex processes that govern it. Many issues remain unsolved even after the MESSENGER mission that ended in 2015. The specific orbits of the two spacecraft, MPO and Mio, and the comprehensive scientific payload allow a wider range of scientific questions to be addressed than those that could be achieved by the individual instruments acting alone, or by previous missions. These joint observations are of key importance because many phenomena in Mercury's environment are highly temporally and spatially variable. Examples of possible coordinated observations are described in this article, analysing the required geometrical conditions, pointing, resolutions and operation timing of different BepiColombo instruments sensors., Comment: 78 pages, 14 figures, published
Published: 2022
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3. Characteristics of Resonant Electrons Interacting With Whistler Waves in the Nearest Dipolarizing Magnetotail

Author: E. V. Panov, David R. Shklyar, Andrei Yu. Malykhin, Levon A. Avanov, O. Le Contel, Elena Grigorenko, Barbara L. Giles, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], 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), NASA Goddard Space Flight Center (GSFC), and University of Graz
Subjects: Physics, 010504 meteorology & atmospheric sciences, Whistler, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Plasma sheet, Electron, 01 natural sciences, Geophysics, Space and Planetary Science, 0103 physical sciences, Atomic physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: The Magnetospheric Multiscale spacecraft observations in the burst mode allow the determination of the characteristics of resonant electrons interacting with quasi-parallel whistler waves during prolonged dipolarizations in the near Earth magnetotail at −22 RE < X ≤ −8 RE. We have detected 163 whistler bursts observed during 48 dipolarization events. The bursts were registered within ∼13 min following the dipolarization onset when the burst mode observations were available. In the majority of events, electrons with energies Wres ≥ 10 keV and pitch angles αres ∼ 100°–130° and αres ∼ 50°–80°made the maximum positive contribution to the growth rate of whistler waves propagating quasi-parallel and antiparallel to the ambient magnetic field, respectively. Our analysis shows that electrons with Wres ∼ 10–20 keV could potentially be scattered into the loss cone by the low frequency whistler waves with fw ∼ (0.05–0.2)fce (fw is the wave frequency and fce is the electron gyrofrequency). The electrons that are scattered into the loss cone can contribute to electron precipitation within ∼13 min following the dipolarization onset. We suggest that whistler waves that are excited due to cyclotron instability driven by the temperature anisotropy of suprathermal electrons (≥2 keV) may, in turn, affect electron distribution in this energy range. Specifically, lower energy resonant electrons transfer a part of their kinetic energy to waves, while more energetic electrons absorb wave energy increasing their kinetic energy. This may lead to the transformation of higher-energy part of electron distribution from Maxwellian to the power law shape.
Published: 2021
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4. STIX X-ray microflare observations during the Solar Orbiter commissioning phase

Author: Andrea Francesco Battaglia, Jonas Saqri, Paolo Massa, Emma Perracchione, Ewan C. M. Dickson, Hualin Xiao, Astrid M. Veronig, Alexander Warmuth, Marina Battaglia, Gordon J. Hurford, Aline Meuris, Olivier Limousin, László Etesi, Shane A. Maloney, Richard A. Schwartz, Matej Kuhar, Frederic Schuller, Valliappan Senthamizh Pavai, Sophie Musset, Daniel F. Ryan, Lucia Kleint, Michele Piana, Anna Maria Massone, Federico Benvenuto, Janusz Sylwester, Michalina Litwicka, Marek Stȩślicki, Tomasz Mrozek, Nicole Vilmer, František Fárník, Jana Kašparová, Gottfried Mann, Peter T. Gallagher, Brian R. Dennis, André Csillaghy, Arnold O. Benz, Säm Krucker, University of Applied Sciences and Arts of Western Switzerland (HES-SO), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institute of Physics [Graz], Karl-Franzens-Universität Graz, Dipartimento di Matematica [Genova], Università degli studi di Genova = University of Genoa (UniGe), Leibniz-Institut für Astrophysik Potsdam (AIP), Univ Paris Diderot, CEA, CNRS, Lab AIM, Gif Sur Yvette, France, Trinity College Dublin, Dublin Institute for Advanced Studies (DIAS), American University Washington D.C. (AU), NASA Goddard Space Flight Center (GSFC), SUPA School of Physics and Astronomy [Glasgow], University of Glasgow, Centre Universitaire d'Informatique (CUI), Université de Genève = University of Geneva (UNIGE), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Astronomical Institute [Wroclaw], University of Wrocław [Poland] (UWr), 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), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
Subjects: Sun: flares, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Orbiter, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Gamma rays, Sun: corona, Sun: X-rays, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, X-ray, Astronomy and Astrophysics, gamma rays, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics
Abstract: The Spectrometer/Telescope for Imaging X-rays (STIX) is the HXR instrument onboard Solar Orbiter designed to observe solar flares over a broad range of flare sizes, between 4-150 keV. We report the first STIX observations of microflares recorded during the instrument commissioning phase in order to investigate the STIX performance at its detection limit. This first result paper focuses on the temporal and spectral evolution of STIX microflares occuring in the AR12765 in June 2020, and compares the STIX measurements with GOES/XRS, SDO/AIA, and Hinode/XRT. For the observed microflares of the GOES A and B class, the STIX peak time at lowest energies is located in the impulsive phase of the flares, well before the GOES peak time. Such a behavior can either be explained by the higher sensitivity of STIX to higher temperatures compared to GOES, or due to the existence of a nonthermal component reaching down to low energies. The interpretation is inconclusive due to limited counting statistics for all but the largest flare in our sample. For this largest flare, the low-energy peak time is clearly due to thermal emission, and the nonthermal component seen at higher energies occurs even earlier. This suggests that the classic thermal explanation might also be favored for the majority of the smaller flares. In combination with EUV and SXR observations, STIX corroborates earlier findings that an isothermal assumption is of limited validity. Future diagnostic efforts should focus on multi-wavelength studies to derive differential emission measure distributions over a wide range of temperatures to accurately describe the energetics of solar flares. Commissioning observations confirm that STIX is working as designed. As a rule of thumb, STIX detects flares as small as the GOES A class. For flares above the GOES B class, detailed spectral and imaging analyses can be performed., Comment: 19 pages, 11 figures
Published: 2021
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5. How Dark Are Radial Breathing Modes in Plasmonic Nanodisks?

Author: Schmidt, Franz-Philipp, Losquin, Arthur, Hofer, Ferdinand, Hohenau, Andreas, Krenn, Joachim, Kociak, Mathieu, Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], Institute for Electron Microscopy and Nanoanalysis [Graz] (IEMN), Graz University of Technology [Graz] (TU Graz), Laboratoire Ondes et Matière d'Aquitaine (LOMA), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Mathematical Physics [Lund], Lund University [Lund], Laboratoire de Physique des Solides (LPS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), European Project: 312483,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2012-1,ESTEEM 2(2012), Karl-Franzens-Universität Graz, and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], electron energy loss spectroscopy, transmission electron microscopy, Physics::Optics, cathodoluminescence, nanoparticles, Article, plasmonics
Abstract: International audience; Due to a vanishing dipole moment, radial breathing modes in small flat plasmonic nanoparticles do not couple to light and have to be probed with a near field source, as in electron energy loss spectroscopy (EELS). With increasing particle size, retardation gives rise to light coupling, enabling probing breathing modes optically or by cathodoluminescence (CL). Here, we investigate single silver nanodisks with diameters of 150−500 nm by EELS and CL in an electron microscope and quantify the EELS/CL ratio, which corre sponds to the ratio of full to radiative damping of the breathing mode. For the investigated diameter range, we find the CL signal to increase by about 1 order of magnitude, in agreement with numerical simulations. Due to reciprocity, our findings corroborate former optical experiments and enable a quantitative understanding of the light coupling of dark plasmonic modes.
Published: 2017
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6. Dust of comet 67P/Churyumov-Gerasimenko collected by Rosetta/MIDAS: classification and extension to the nanometer scale

Author: Thurid Mannel, Mark Bentley, Pascale Ehrenfreund, Klaus Torkar, J. Romstedt, Peter Boakes, Iris Weber, Cécile Engrand, H. Jeszenszky, Christian Koeberl, Roland Schmied, Anny Chantal Levasseur-Regourd, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institute of Physics [Graz], University of Graz, European Space Astronomy Centre (ESAC), European Space Agency (ESA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Space Policy Institute [Washington], The George Washington University (GW), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Lithospheric Research [Wien], Universität Wien, Natural History Museum [Vienna] (NHM), 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), European Space Research and Technology Centre (ESTEC), Institut für Weltraumforschung [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), Karl-Franzens-Universität [Graz, Autriche], and Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Planetesimal, Range (particle radiation), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Comet, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, 01 natural sciences, Fractal dimension, Interplanetary dust cloud, 13. Climate action, Space and Planetary Science, Agglomerate, 0103 physical sciences, Particle, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: Context. The properties of the smallest subunits of cometary dust contain information on their origin and clues to the formation of planetesimals and planets. Compared to interplanetary dust particles or particles collected during the Stardust mission, dust collected in the coma of comet 67P/Churyumov-Gerasimenko (67P) during the Rosetta mission provides a resource of minimally altered material with known origin whose structural properties can be used to further the investigation of the early solar system. Aims. The cometary dust particle morphologies found at comet 67P on the micrometer scale are classified, and their structural analysis is extended to the nanometer scale. Methods. We present a novel method for achieving the highest spatial resolution of imaging obtained with the MIDAS Atomic Force Microscope on board Rosetta. 3D topographic images with resolutions down to 8 nm were analyzed to determine the subunit sizes of particles on the nanometer scale. Results. Three morphological classes can be determined: (i) fragile agglomerate particles of sizes larger than about 10 μm comprised of micrometer-sized subunits that may themselves be aggregates and show a moderate packing density on the surface of the particles. (ii) A fragile agglomerate with a size of about a few tens of micrometers comprised of micrometer-sized subunits that are suggested to be aggregates themselves and are arranged in a structure with a fractal dimension lower than two. (iii) Small micrometer-sized particles comprised of subunits in the size range of hundreds of nanometers that show surface features that are again suggested to represent subunits. Their differential size distributions follow a log-normal distribution with means of about 100 nm and standard deviations between 20 and 35 nm. Conclusions. The properties of the dust particles found by MIDAS represent an extension of the dust results of Rosetta to the micro- and nanometer scale. All micrometer-sized particles are hierarchical dust agglomerates of smaller subunits. The arrangement, appearance, and size distribution of the smallest determined surface features are reminiscent of those found in chondritic porous interplanetary dust particles. They represent the smallest directly detected subunits of comet 67P.
Published: 2019
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7. Modeling the multiple CME interaction event on 6-9 September 2017 with WSA-ENLIL+Cone

Author: Andrew Dimmock, Emiliya Yordanova, Manuela Temmer, A. L. E. Werner, HELIOS - 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), Swedish Institute of Space Physics [Uppsala] (IRF), Institute of Physics [Graz], and Karl-Franzens-Universität [Graz, Autriche]
Subjects: Physics, Atmospheric Science, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Interplanetary medium, Astrophysics, 01 natural sciences, Arrival time, law.invention, Shock (mechanics), Solar wind, law, 0103 physical sciences, Coronal mass ejection, Interplanetary spaceflight, 010303 astronomy & astrophysics, Coronagraph, Event (particle physics), 0105 earth and related environmental sciences
Abstract: International audience; A series of coronal mass ejections (CMEs) erupted from the same active region between 4‐6 September 2017. Later, on 6‐9 September, two interplanetary (IP) shocks reached L1, creating a complex and geoeffective plasma structure. To understand the processes leading up to the formation of the two shocks, we model the CMEs with the Wang‐Sheeley‐Arge (WSA)‐ENLIL+Cone model. The first two CMEs merged already in the solar corona driving the first IP shock. In interplanetary space, another fast CME presumably interacted with the flank of the preceding CMEs and caused the second shock detected in‐situ. By introducing a customized density enhancement factor (dcld) in the WSA‐ENLIL+Cone model based on coronagraph image observations, the predicted arrival time of the first IP shock was drastically improved. When the dcld factor was tested on a well‐defined single CME event from 12 July 2012 the shock arrival time saw similar improvement. These results suggest that the proposed approach may be an alternative to improve the forecast for fast and simple CMEs. Further, the slowly decelerating kilometric type II radio burst confirm the properties of the background solar wind have been preconditioned by the passage of the first IP shock. This likely caused the last CME to experience insignificant deceleration and led to the early arrival of the second IP shock. This result emphasizes the need to take preconditioning of the interplanetary medium into account when making forecasts of CMEs erupting in quick succession.
Published: 2019
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8. Synthesis of the morphological description of cometary dust at comet 67P/Churyumov-Gerasimenko

Author: Martin Hilchenbach, Klaus Hornung, Alberto Flandes, Jérémie Lasue, Anny Chantal Levasseur-Regourd, Giovanna Rinaldi, Stavro Ivanovski, Marco Fulle, Harald Krüger, Andrea Longobardo, Dominique Bockelée-Morvan, Dennis Bodewits, Stefano Mottola, Yves Langevin, C. Güttler, Gianrico Filacchione, Ivano Bertini, G. P. Tozzi, Holger Sierks, Jürgen Blum, J. Agarwal, Fabrizio Capaccioni, Giampiero Naletto, Thurid Mannel, F. Moreno, Alessandra Rotundi, Imre Tóth, Sihane Merouane, V. Della Corte, John Paquette, Cecilia Tubiana, Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Max-Planck-Institut für Sonnensystemforschung (MPS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Dipartimento di Scienze e Tecnologie [Napoli] (DIST), Universita degli studi di Napoli 'Parthenope' [Napoli], INAF - Osservatorio Astronomico di Trieste (OAT), 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), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Dipartimento di Fisica e Astronomia 'Galileo Galilei', CNR Istituto di Fotonica e Nanotecnologie [Milano] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), Instituto de Geofisica [Mexico], Universidad Nacional Autónoma de México (UNAM), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics [Auburn], Auburn University (AU), INAF - Osservatorio Astrofisico di Arcetri (OAA), Universität der Bundeswehr München [Neubiberg], Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Karl-Franzens-Universität Graz, Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -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)-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), Università degli Studi di Padova = University of Padua (Unipd), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Graz, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), IMPEC - LATMOS, Technische Universität Braunschweig [Braunschweig], Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ITA, FRA, DEU, and ESP
Subjects: Asteroiden und Kometen, instruments [space vehicles], 010504 meteorology & atmospheric sciences, comets: general – comets: individual: 67P/Churyumov-Gerasimenko – space vehicles: instruments, Computer science, Comet, Individual, 01 natural sciences, Space exploration, Astrobiology, Interplanetary dust cloud, individual: 67P/Churyumov-Gerasimenko [Comets], 0103 physical sciences, 67P/Churyumov-Gerasimenko - space vehicles, Comets, General - comets, Instruments, Instrumentation (computer programming), space vehicles: instruments, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Comets: individual: 67P/Churyumov-Gerasimenko, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], general [Comets], Astronomy and Astrophysics, Common framework, Comets: general, [SDU]Sciences of the Universe [physics], Space and Planetary Science
Abstract: Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society., Before Rosetta, the space missions Giotto and Stardust shaped our view on cometary dust, supported by plentiful data from Earth based observations and interplanetary dust particles collected in the Earth's atmosphere. The Rosetta mission at comet 67P/Churyumov-Gerasimenko was equipped with a multitude of instruments designed to study cometary dust. While an abundant amount of data was presented in several individual papers, many focused on a dedicated measurement or topic. Different instruments, methods, and data sources provide different measurement parameters and potentially introduce different biases. This can be an advantage if the complementary aspect of such a complex data set can be exploited. However, it also poses a challenge in the comparison of results in the first place. The aim of this work therefore is to summarize dust results from Rosetta and before. We establish a simple classification as a common framework for intercomparison. This classification is based on the dust particle structure, porosity, and strength and also on its size. Depending on the instrumentation, these are not direct measurement parameters, but we chose them because they were the most reliable for deriving our model. The proposed classification has proved helpful in the Rosetta dust community, and we offer it here also for a broader context. In this manner, we hope to better identify synergies between different instruments and methods in the future.© C. Güttler et al. 2019
Published: 2019
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9. Coulomb correlations in 4d and 5d oxides from first principles—or how spin–orbit materials choose their effective orbital degeneracies

Author: Martins, Cyril, Aichhorn, Markus, Biermann, Silke, Systèmes étendus et magnétisme (LCPQ) (SEM), Laboratoire de Chimie et Physique Quantiques (LCPQ), Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut de Chimie du CNRS (INC)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut de Chimie du CNRS (INC), Department of Theoretical Physics [Graz], Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche]-Karl-Franzens-Universität [Graz, Autriche], Centre de Physique Théorique [Palaiseau] (CPHT), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse)
Subjects: Condensed Matter - Strongly Correlated Electrons, Strongly Correlated Electrons (cond-mat.str-el), FOS: Physical sciences, [PHYS.COND.CM-SCE]Physics [physics]/Condensed Matter [cond-mat]/Strongly Correlated Electrons [cond-mat.str-el], ComputingMilieux_MISCELLANEOUS
Abstract: The interplay of spin-orbit interactions and Coulomb correlations has become a hot topic in condensed matter theory. Here, we review recent advances in dynamical mean-field theory-based electronic structure calculations for iridates and rhodates. We stress the notion of the effective degeneracy of the compounds, which introduces an additional axis into the conventional picture of a phase diagram based on filling and on the ratio of interactions to bandwidth., 45 pages, 9 figures in \Psi_k Scientific Highlight Of The Month 132 (Novembre 2016)
Published: 2017
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10. How MIDAS improved our understanding of micrometre- sized cometary dust

Author: Mannel, Thurid, Bentley, Mark Stephen, Boakes, Peter, Jeszenszky, Harald, Levasseur-Regourd, Anny Chantal, Schmied, Roland, Torkar, Klaus, Cardon, Catherine, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], PLANETO - 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), and Karl-Franzens-Universität Graz
Subjects: [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; The MIDAS atomic force microscope on the Rosetta orbiter was an instrument developed to investigate, for the first time, the morphology of nearly unaltered cometary dust. It acquired the 3D topography of about 1-50 µm sized dust particles with resolutions down to a few nanometres. These images showed the agglomerate character of the dust and confirmed that the smallest subunit sizes were less than 100 nm. MIDAS acquired the first direct proof of a fractal dust particle, opening a new approach to investigate the history of our early Solar System and of comets.
Published: 2017

11. The 2016 Feb 19 outburst of comet 67P/CG: an ESA Rosetta multi-instrument study

Author: Andrew J. Steffl, Harold A. Weaver, Lori M. Feaga, Paul R. Weissman, B. J. R. Davidsson, Francesco Marzari, Chia-Yu Tzou, Roberto Sordini, J. L. Bertaux, Philippe Lamy, Michaël Gillon, Hans Rickman, P. Yanamandra-Fisher, Matthew M. Knight, O. Mousis, Nicolas Altobelli, Sonia Fornasier, Jessica Agarwal, Marco Fulle, Marina Galand, A. I. Erikson, J. J. López-Moreno, Eric Schindhelm, Mihaly Horanyi, Charlotte Götz, James L. Burch, Giampiero Naletto, Kathrin Altwegg, E. Mazzotta Epifani, Jean Manfroid, Mark Bentley, Jörg Knollenberg, Emmanuel Jehin, Ekkehard Kührt, M Muller, M. A. Barucci, Cesare Barbieri, Pierre Henri, V. Della Corte, P. J. Gutiérrez, Stavro Ivanovski, Carsten Güttler, Harald Krüger, Ralf Srama, Cecilia Tubiana, Rafael Rodrigo, F. Schmidt, J. E. Rodriguez, Vladimir Zakharov, J.-R. Kramm, Roland Schmied, S. A. Stern, Eberhard Grün, Thurid Mannel, Jakob Deller, A. Gicquel, Colin Snodgrass, Bernhard Geiger, M. De Cecco, B. Grieger, Monica Lazzarin, Seungwon Lee, Wing-Huen Ip, Laurent Jorda, Holger Sierks, Stubbe F. Hviid, Marc Hofmann, Paul D. Feldman, J. Wm. Parker, M. Sommer, Michael Küppers, Matthew Taylor, M. F. A'Hearn, Olivier Groussin, Simon F. Green, Detlef Koschny, Nicolas Thomas, Horst Uwe Keller, Cyrielle Opitom, Gabriele Cremonese, Niklas J. T. Edberg, Mark Hofstadter, R. H. Soja, M. Ferrari, E. Morales, Ivano Bertini, N. Biver, Pasquale Palumbo, Nilda Oklay, Stefano Debei, V. Da Deppo, L. M. Lara, Luigi Colangeli, Alessandra Rotundi, Xian Shi, J. B. Vincent, Science and Technology Facilities Council (STFC), Centre National de la Recherche Scientifique (France), German Centre for Air and Space Travel, Agenzia Spaziale Italiana, Swedish National Space Board, European Space Agency, Ministerio de Economía y Competitividad (España), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Swedish Institute of Space Physics [Uppsala] (IRF), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Imperial College London, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Jaicoa Observatory, 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), European Space Operations Center (ESOC), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Institute of Physics [Graz], Karl-Franzens-Universität Graz, Institut für Raumfahrtsysteme (IRS), Universität Stuttgart [Stuttgart], 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), Space Science Institute [Boulder] (SSI), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), PLANETO - 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), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), European Space Research and Technology Centre (ESTEC), INAF - Osservatorio Astronomico di Padova (OAPD), CNR Institute for Photonics and Nanotechnologies (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Department of Physics and Astronomy [Uppsala], Uppsala University, Department of Industrial Engineering [Padova], INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), Operations Department (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Department of Information Engineering [Padova] (DEI), SwRI Planetary Science Directorate [Boulder], Southwest Research Institute [Boulder] (SwRI), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), International Space Science Institute [Bern] (ISSI), Department of Space Studies [Boulder], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Planetary Science Institute [Tucson] (PSI), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Agence Nationale de la Recherche (ANR), ANR-15-CE31-0009,SPECTRA,Sonder le Plasma dans l'Environnement d'une ComètE avec RosettA(2015), ANR-11-IDEX-0001,Amidex,INITIATIVE D'EXCELLENCE AIX MARSEILLE UNIVERSITE(2011), Max-Planck-Institut für Sonnensystemforschung (MPS), European Space Agency (ESA), Universität Bern [Bern], Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), 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), Universita degli studi di Napoli 'Parthenope' [Napoli], Karl-Franzens-Universität [Graz, Autriche], Universita degli Studi di Padova, Consiglio Nazionale delle Ricerche [Roma] (CNR), European Space Agency (ESA)-European Space Agency (ESA), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), ITA, USA, GBR, FRA, DEU, and ESP
Subjects: 67P/Churyumov-Gerasimenko, Brightness, Electron density, 010504 meteorology & atmospheric sciences, 530 Physics, 67P/Churyumov-gerasimenko, Comets, Individual, Astronomy and Astrophysics, Space and Planetary Science, Comet, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Astronomi, astrofysik och kosmologi, law, Dust collector, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, Astronomy, comets: individual: 67P/Churyumov-Gerasimenko, Radius, 620 Engineering, Wavelength, 0201 Astronomical And Space Sciences, 13. Climate action, Magnitude (astronomy), individual: 67P/Churyumov-Gerasimenko [comets]
Abstract: On 2016 Feb 19, nine Rosetta instruments serendipitously observed an outburst of gas and dust from the nucleus of comet 67P/Churyumov-Gerasimenko. Among these instruments were cameras and spectrometers ranging from UV over visible to microwave wavelengths, in situ gas, dust and plasma instruments, and one dust collector. At 09:40 a dust cloud developed at the edge of an image in the shadowed region of the nucleus. Over the next two hours the instruments recorded a signature of the outburst that significantly exceeded the background. The enhancement ranged from 50 per cent of the neutral gas density at Rosetta to factors >100 of the brightness of the coma near the nucleus. Dust related phenomena (dust counts or brightness due to illuminated dust) showed the strongest enhancements (factors>10). However, even the electron density at Rosetta increased by a factor 3 and consequently the spacecraft potential changed from ~-16 V to -20 V during the outburst. A clear sequence of events was observed at the distance of Rosetta (34 km from the nucleus): within 15 min the Star Tracker camera detected fast particles (~25 m s-1) while 100 ¿m radius particles were detected by the GIADA dust instrument ~1 h later at a speed of 6 m s-1. The slowest were individual mm to cm sized grains observed by the OSIRIS cameras. Although the outburst originated just outside the FOV of the instruments, the source region and the magnitude of the outburst could be determined. © 2016 The Authors., Rosetta is an ESA mission with contributions from its member states and NASA. Rosetta's Philae lander is provided by a consortium led by DLR, MPS, CNES and ASI. We thank all elements of the Rosetta project for the magnificent job they are doing to make this mission an astounding success. The Alice team acknowledges continuing support from NASA's Jet Propulsion Laboratory through contract 1336850. GIADA/Univ Parthenope NA/INAFOAC/IAA/INAF-IAPS: this research was supported by the Italian Space Agency (ASI) within the ASI-INAF agreements I/032/05/0 and I/024/12/0. OSIRIS was built by a consortium of the Max-Planck- Institut für Sonnensystemforschung, Göttingen, Germany, CISAS University of Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the Instituto de Astrofìsica de Andalucia, CSIC, Granada, Spain, the Research and Scientific Support Department of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Técnica Aeroespacial, Madrid, Spain, the Universidad Politéechnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, the UK(STFC), and the Institut für Datentechnik und Kommunikationsnetze der Technischen Universität Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France(CNES), Italy(ASI), Spain(MEC), Sweden(SNSB), and the ESA Technical Directorate is gratefully acknowledged. Work at LPC2E/CNRS was supported by CNES and by ANR under the financial agreement ANR-15-CE31-0009-01. Work on ROSINA COPS at the University of Bern was funded by the State of Bern, the Swiss National Science Foundation and by the European Space Agency PRODEX program. OM: this work has been partly carried out thanks to the support of the A*MIDEX project (no ANR-11-IDEX-0001-02) funded by the ‘Investissements d'Avenir’ French Government program, managed by the French National Research Agency (ANR). This work also benefited from the support of CNRS-INSU national program for planetology (PNP).
Published: 2016
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12. Aggregate dust particles at comet 67P/Churyumov–Gerasimenko

Author: H. Jeszenszky, Ove Havnes, Pascale Ehrenfreund, Christian Koeberl, Mark Bentley, Thurid Mannel, J. Romstedt, Roland Schmied, Iris Weber, Klaus Torkar, Elmar K. Jessberger, Anny Chantal Levasseur-Regourd, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institute of Physics [Graz], University of Graz, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), PLANETO - 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), Universidade Federal de Pernambuco [Recife] (UFPE), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), Space Policy Institute [Washington], The George Washington University (GW), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Natural History Museum [Vienna] (NHM), Department of Lithospheric Research [Wien], Universität Wien, Tromsø Geophysical Observatory (TGO), The Arctic University of Norway (UiT), Department of Physics and Technology [Tromsø], University of Tromsø (UiT), Karl-Franzens-Universität [Graz, Autriche], Karl-Franzens-Universität Graz, Agence Spatiale Européenne = European Space Agency (ESA), Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Universiteit Leiden, and The Arctic University of Norway [Tromsø, Norway] (UiT)
Subjects: 010504 meteorology & atmospheric sciences, Comet dust, Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, Astrobiology, Kuiper belt, Interplanetary dust cloud, 0103 physical sciences, comets, Early solar system, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Cosmic dust, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, Asteroids, Particle aggregation, 13. Climate action, Asteroid, Agglomerate, Formation and evolution of the Solar System, Astrophysics - Earth and Planetary Astrophysics
Abstract: International audience; Comets are thought to preserve almost pristine dust particles, thus providing a unique sample of the properties of the early solar nebula. The microscopic properties of this dust played a key part in particle aggregation during the formation of the Solar System1, 2. Cometary dust was previously considered to comprise irregular, fluffy agglomerates on the basis of interpretations of remote observations in the visible and infrared3, 4, 5, 6 and the study of chondritic porous interplanetary dust particles7 that were thought, but not proved, to originate in comets. Although the dust returned by an earlier mission8 has provided detailed mineralogy of particles from comet 81P/Wild, the fine-grained aggregate component was strongly modified during collection9. Here we report in situ measurements of dust particles at comet 67P/Churyumov–Gerasimenko. The particles are aggregates of smaller, elongated grains, with structures at distinct sizes indicating hierarchical aggregation. Topographic images of selected dust particles with sizes of one micrometre to a few tens of micrometres show a variety of morphologies, including compact single grains and large porous aggregate particles, similar to chondritic porous interplanetary dust particles. The measured grain elongations are similar to the value inferred for interstellar dust and support the idea that such grains could represent a fraction of the building blocks of comets. In the subsequent growth phase, hierarchical agglomeration could be a dominant process10 and would produce aggregates that stick more easily at higher masses and velocities than homogeneous dust particles11. The presence of hierarchical dust aggregates in the near-surface of the nucleus of comet 67P also provides a mechanism for lowering the tensile strength of the dust layer and aiding dust release12.
Published: 2016
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13. TRIQS/DFTTools: A TRIQS application for ab initio calculations of correlated materials

Author: Jernej Mravlje, Markus Aichhorn, Leonid Pourovskii, Verónica Vildosola, Olivier Parcollet, Xiaoyu Deng, Manuel Zingl, Gernot J. Kraberger, Priyanka Seth, Oleg E. Peil, Michel Ferrero, Cyril Martins, Department of Theoretical Physics [Graz], Institute of Physics [Graz], Karl-Franzens-Universität Graz-Karl-Franzens-Universität Graz, Centre de Physique Théorique [Palaiseau] (CPHT), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Physique de la matière condensée (A. Georges), Collège de France (CdF (institution)), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Jozef Stefan Institute [Ljubljana] (IJS), Systèmes étendus et magnétisme (LCPQ) (SEM), Laboratoire de Chimie et Physique Quantiques (LCPQ), Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), European Project: 617196,EC:FP7:ERC,ERC-2013-CoG,CORRELMAT(2014), European Project: 278472,EC:FP7:ERC,ERC-2011-StG_20101014,MOTTMETALS(2012), Karl-Franzens-Universität [Graz, Autriche]-Karl-Franzens-Universität [Graz, Autriche], Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Chaire Physique de la matière condensée (A. Georges), University of Geneva [Switzerland], Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse)
Subjects: ab-initio calculations, Computer science, Interface (Java), Ciencias Físicas, Ab initio, General Physics and Astronomy, FOS: Physical sciences, 02 engineering and technology, 01 natural sciences, Computational science, WIEN2k, Condensed Matter - Strongly Correlated Electrons, Ab initio quantum chemistry methods, 0103 physical sciences, 010306 general physics, Electronic band structure, Strongly-correlated electrons, Basis set, [PHYS]Physics [physics], Wannier function, Condensed Matter - Materials Science, Strongly Correlated Electrons (cond-mat.str-el), Materials Science (cond-mat.mtrl-sci), 021001 nanoscience & nanotechnology, Computational physics, Dynamical mean-field theory, Many-body physics, Hardware and Architecture, Density functional theory, 0210 nano-technology, CIENCIAS NATURALES Y EXACTAS, Física de los Materiales Condensados
Abstract: We present the TRIQS/DFTTools package, an application based on the TRIQS library that connects this toolbox to realistic materials calculations based on density functional theory (DFT). In particular, TRIQS/DFTTools together with TRIQS allows an efficient implementation of DFT plus dynamical mean-field theory (DMFT) calculations. It supplies tools and methods to construct Wannier functions and to perform the DMFT self-consistency cycle in this basis set. Post-processing tools, such as band-structure plotting or the calculation of transport properties are also implemented. The package comes with a fully charge self-consistent interface to the Wien2k band structure code, as well as a generic interface that allows to use TRIQS/DFTTools together with a large variety of DFT codes. It is distributed under the GNU General Public License (GPLv3)., Comment: 18 pages, 6 figures, Comp. Phys. Comm. accepted version
Published: 2016
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14. Similar behaviors of natural ELF/VLF ionospheric emissions and transmitter signals over seismic Adriatic regions

Author: Ö. Aydogar, Mohammed Y. Boudjada, J. Weingrill, Jan Blecki, G. Stangl, Konrad Schwingenschuh, H. K. Biernat, Manfred Stachel, Michel Parrot, Jean-Jacques Berthelier, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Department of Theoretical Physics [Graz], Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche]-Karl-Franzens-Universität [Graz, Autriche], Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Austrian Federal Office for Metrology and Surveying (BEV), and Austrian Federal Ministry of Economics and Labour
Subjects: 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDE.MCG]Environmental Sciences/Global Changes, 0211 other engineering and technologies, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], 02 engineering and technology, 01 natural sciences, Signal, lcsh:TD1-1066, Physics::Geophysics, Large earthquakes, Spectral analysis, lcsh:Environmental technology. Sanitary engineering, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, lcsh:Environmental sciences, 0105 earth and related environmental sciences, lcsh:GE1-350, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, 021110 strategic, defence & security studies, lcsh:QE1-996.5, Transmitter, lcsh:Geography. Anthropology. Recreation, Geophysics, lcsh:Geology, On board, Earth's magnetic field, lcsh:G, 13. Climate action, Physics::Space Physics, General Earth and Planetary Sciences, Ionosphere, Seismology, Geology
Abstract: We report on the analysis of ELF/VLF emissions observed by the Instrument Champ Electrique (ICE) experiment onboard the DEMETER micro-satellite. We consider principally selected seismic events reported by Molchanov et al. (2006). These authors studied the VLF signals radiated by ground transmitters and received on board the DEMETER micro-satellite. They revealed a drop of the signals (scattering spot) connected with the occurrence of large earthquakes. In our investigations, we proceed to a spectral analysis of ICE observations with the aim to find if the natural ionospheric VLF/ELF emissions show, or not, a similar ''drop'' in the intensity as it is the case of the VLF transmitter signal. We combine our results with those of Molchanov et al. (2006), and we discuss the origin of such interesting ionospheric features in the frame of the investigation of the pre-seismic electromagnetic emissions. We show that the geomagnetic activity is a key parameter which could disturb the natural VLF ionospheric emissions, and also the transmitter signal. We find that it is not possible to conclude the presence, or not, of a preseismic effect when the Kp-index is higher than one.
Published: 2008
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15. Fractal cometary dust – a window into the early Solar System

Author: Klaus Torkar, Roland Schmied, Thurid Mannel, H. Jeszenszky, J. Romstedt, Mark Bentley, Anny Chantal Levasseur-Regourd, Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), PLANETO - 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), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), University of Graz, Karl-Franzens-Universität Graz, and Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: Physics, Planetesimal, education.field_of_study, 010504 meteorology & atmospheric sciences, Comet, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, Astronomy and Astrophysics, Astrophysics, Protoplanetary disk, 01 natural sciences, Fractal dimension, Fractal analysis, Fractal, Interplanetary dust cloud, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The ESLAB 50 Symposium - spacecraft at comets from 1P/Halley to 67P/Churyumov-Gerasimenko; International audience; The properties of dust in the protoplanetary disk are key to understanding the formation of planets in our Solar System. Many models of dust growth predict the development of fractal structures that evolve into non-fractal, porous dust pebbles representing the main component for planetesimal accretion. In order to understand comets and their origins, the Rosetta orbiter followed comet 67P/Churyumov-Gerasimenko for over two years and carried a dedicated instrument suite for dust analysis. One of these instruments, the MIDAS atomic force microscope, recorded the 3D topography of micro- to nanometre sized dust. All particles analysed to date have been found to be hierarchical agglomerates. Most show compact packing, however, one is extremely porous. This paper contains a structural description of a compact aggregate and the outstanding porous one. Both particles are tens of micrometres in size and show rather narrow subunit size distributions with noticeably similar mean values of 1.48+0.13−0.59 μm for the porous particle and 1.36+0.15−0.59 μm for the compact. ompact. The porous particle allows a fractal analysis, where a density-density correlation function yields a fractal dimension of Df = 1.70 ± 0.1. GIADA, another dust analysis instrument on-board Rosetta, confirms the existence of a dust population with a similar fractal dimension. The fractal particles are interpreted as pristine agglomerates built in the protoplanetary disk and preserved in the comet. The similar subunits of both fractal and compact dust indicate a common origin which is, given the properties of the fractal, dominated by slow agglomeration of equally sized aggregates known as cluster-cluster agglomeration.
Published: 2016
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16. The PAC2MAN mission: a new tool to understand and predict solar energetic events

Author: Sophie Musset, Jorge Amaya, René Kiefer, Solène Lejosne, Mirko Rummelhagen, Andrea Diercke, Christian Höller, Riccardo Lasagni, S. Thonhofer, Viktor Andersson, Lilla Juhász, Mohammad Madi, Sergiu Iliev, Markus Scheucher, Arianna Sorba, Centre for Mathematical Plasma-Astrophysics [Leuven] (CmPA), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), 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), Swedish Institute of Space Physics [Kiruna] (IRF), Leibniz-Institut für Astrophysik Potsdam (AIP), Institut für Physik und Astrophysik [Potsdam], University of Potsdam = Universität Potsdam, Faculty of Mechanical and Industrial Engineering, Department for Space Mechanisms, Aeronautical Engineering Department, Imperial College London, Department of Geophysics and Space Research [Budapest], Eötvös Loránd University (ELTE), Kiepenheuer-Institut für Sonnenphysik (KIS), Department of Aerospace Engineering, British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Micos Engineering GmbH, Berner & Mattner Systemtechnik, Institute of Physics [Graz], Karl-Franzens-Universität Graz, Blackett Laboratory, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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), Universität Potsdam, Karl-Franzens-Universität [Graz, Autriche], and Jorge Amaya, Sophie Musset, Viktor Andersson, Andrea Diercke, Christian Höller, Sergiu Iliev, Lilla Juhász, René Kiefer, Riccardo Lasagni, Solène Lejosne, Mohammad Madi, Mirko Rummelhagen, Markus Scheucher, Arianna Sorba, Stefan Thonhofer
Subjects: Atmospheric Science, Space weather, FOS: Physical sciences, Mission, lcsh:QC851-999, 7. Clean energy, Missions, Coronal mass ejection (CME), Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Spacecraft, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physics::Atmospheric and Oceanic Physics, Remote sensing, Physics, Solar conjunction, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Coronal loop, Solar wind, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, lcsh:Meteorology. Climatology, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Heliocentric orbit, Flare, Space environment
Abstract: An accurate forecast of flare and CME initiation requires precise measurements of the magnetic energy build up and release in the active regions of the solar atmosphere. We designed a new space weather mission that performs such measurements using new optical instruments based on the Hanle and Zeeman effects. The mission consists of two satellites, one orbiting the L1 Lagrangian point (Spacecraft Earth, SCE) and the second in heliocentric orbit at 1AU trailing the Earth by 80$^\circ$ (Spacecraft 80, SC80). Optical instruments measure the vector magnetic field in multiple layers of the solar atmosphere. The orbits of the spacecraft allow for a continuous imaging of nearly 73\% of the total solar surface. In-situ plasma instruments detect solar wind conditions at 1AU and ahead of our planet. Earth directed CMEs can be tracked using the stereoscopic view of the spacecraft and the strategic placement of the SC80 satellite. Forecasting of geoeffective space weather events is possible thanks to an accurate surveillance of the magnetic energy build up in the Sun, an optical tracking through the interplanetary space, and in-situ measurements of the near-Earth environment., Accepted for publication in the Journal of Space Weather and Space Climate (SWSC)
Published: 2014
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17. Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

Author: I. W. Kienreich, Olga Malandraki, Karl-Ludwig Klein, Astrid Veronig, Rositsa Miteva, Manuela Temmer, Space Research and Technology Institute [Sofia], Bulgarian Academy of Sciences (BAS), 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), Institute of Physics [Graz], Karl-Franzens-Universität Graz, Demokritos University of Thrace, Department of Electrical Engineering, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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), and Karl-Franzens-Universität [Graz, Autriche]
Subjects: Physics, [PHYS]Physics [physics], Solar energetic particles, Proton, FOS: Physical sciences, Solar cycle 23, Astronomy and Astrophysics, Astrophysics, Electron, Corona, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Coronal mass ejection, Extreme ultraviolet Imaging Telescope, Astrophysics::Solar and Stellar Astrophysics, Heliospheric current sheet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS
Abstract: We explore the link between solar energetic particles (SEPs) observed at 1 AU and large-scale disturbances propagating in the solar corona, named after the Extreme ultraviolet Imaging Telescope (EIT) as EIT waves, which trace the lateral expansion of a coronal mass ejection (CME). A comprehensive search for SOHO/EIT waves was carried out for 179 SEP events during Solar Cycle 23 (1997 – 2006). 87 % of the SEP events were found to be accompanied by EIT waves. In order to test if the EIT waves play a role in the SEP acceleration, we compared their extrapolated arrival time at the footpoint of the Parker spiral with the particle onset in the 26 eastern SEP events that had no direct magnetic connection to the Earth. We find that the onset of proton events was generally consistent with this scenario. However, in a number of cases the first near-relativistic electrons were detected too early. Furthermore, the electrons had in general only weakly anisotropic pitch-angle distributions. This poses a problem for the idea that the SEPs were accelerated by the EIT wave or in any other spatially confined region in the low corona. The presence of weak electron anisotropies in SEP events from the eastern hemisphere suggests that transport processes in interplanetary space, including cross-field diffusion, play a role in giving the SEPs access to a broad range of helio-longitudes.
Published: 2014
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18. Initiation of Coronal Mass Ejections by Sunspot Rotation

Author: Tibor Torok, Astrid Veronig, Manuela Temmer, Bojan Vršnak, Gherardo Valori, Lidia van Driel-Gesztelyi, Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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), 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), Physique solaire, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Karl-Franzens-Universität Graz, University of Graz, and 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)
Subjects: 010504 meteorology & atmospheric sciences, Field (physics), Magnetic fields - corona, Active regions - models, Coronal mass ejections - initiation and propagation, Sunspots - velocity, FOS: Physical sciences, Astrophysics, Rotation, 01 natural sciences, law.invention, Protein filament, law, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Sunspot, Astronomy and Astrophysics, Magnetic field, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Magnetohydrodynamics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Flare
Abstract: We study a filament eruption, two-ribbon flare, and coronal mass ejection (CME) that occurred in Active Region NOAA 10898 on 6 July 2006. The filament was located South of a strong sunspot that dominated the region. In the evolution leading up to the eruption, and for some time after it, a counter-clockwise rotation of the sunspot of about 30 degrees was observed. We suggest that the rotation triggered the eruption by progressively expanding the magnetic field above the filament. To test this scenario, we study the effect of twisting the initially potential field overlying a pre-existing flux-rope, using three-dimensional zero-$\beta$ MHD simulations. We first consider a relatively simple and symmetric system, and then study a more complex and asymmetric magnetic configuration, whose photospheric flux distribution and coronal structure are guided by the observations and a potential field extrapolation. In both cases, we find that the twisting leads to the expansion of the overlying field. As a consequence of the progressively reduced magnetic tension, the flux-rope quasi-statically adapts to the changed environmental field, rising slowly. Once the tension is sufficiently reduced, a distinct second phase of evolution occurs where the flux-rope enters an unstable regime characterized by a strong acceleration. Our simulations thus suggest a new mechanism for the triggering of eruptions in the vicinity of rotating sunspots., Comment: 28 pages, 10 figures
Published: 2013
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19. Edge scattering of surface plasmons excited by scanning tunneling microscopy

Author: Tao Wang, Yang Zhang, Gérald Dujardin, Geneviève Comtet, Andreas Hohenau, Joachim R. Krenn, Benoît Rogez, Eric Le Moal, Elizabeth Boer-Duchemin, Christian Gruber, Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Photophysique Moléculaire (PPM), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], ANR project NAPHO (contract ANR-08-NANO-054), European STREP ARTIST (contract FP7 243421), ESF travel grant (PLASMON BIONANOSENSE), ANR-08-NANO-0054,NAPHO,Nanocomposites à propriétés piézoélectriques et optiques(2008), European Project: 243421,EC:FP7:ICT,FP7-ICT-2009-C,ARTIST(2010), Karl-Franzens-Universität Graz, and University of Graz
Subjects: Light, Forward scatter, Physics::Optics, 02 engineering and technology, 01 natural sciences, law.invention, Optics, Microscopy, Scanning Tunneling, law, 0103 physical sciences, Scattering, Radiation, OCIS: 240.6680, 250.5403, 240.7040, 300.2140, Wave vector, 010306 general physics, Plasmon, Physics, Total internal reflection, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], Scattering, business.industry, Surface plasmon, Equipment Design, Surface Plasmon Resonance, 021001 nanoscience & nanotechnology, Surface plasmon polariton, Atomic and Molecular Physics, and Optics, Equipment Failure Analysis, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Gold, Scanning tunneling microscope, 0210 nano-technology, business
Abstract: International audience; The scattering of electrically excited surface plasmon polaritons (SPPs) into photons at the edges of gold metal stripes is investigated. The SPPs are locally generated by the inelastic tunneling current of a scanning tunneling microscope (STM). The majority of the collected light arising from the scattering of SPPs at the stripe edges is emitted in the forward direction and is collected at large angle (close to the air-glass critical angle, θ c). A much weaker isotropic component of the scattered light gives rise to an interference pattern in the Fourier plane images, demonstrating that plasmons may be scattered coherently. An analysis of the interference pattern as a function of excitation position on the stripe is used to determine a value of 1.42 ± 0.18 for the relative plasmon wave vector (k SPP /k 0) of the corresponding SPPs. From these results, we interpret the directional, large angle (θ~θ c) scattering to be mainly from plasmons on the air-gold interface, and the diffuse scattering forming interference fringes to be dominantly from plasmons on the gold-substrate interface.
Published: 2013
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20. Hallmark of strong electronic correlations in LaNiO3: Photoemission kink and broadening of fully occupied bands

Author: Antoine Georges, Michel Ferrero, Markus Aichhorn, Xiaoyu Deng, Jernej Mravlje, Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique [Palaiseau] (CPHT), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Chaire Physique de la matière condensée (A. Georges), Collège de France (CdF (institution)), Jozef Stefan Institute [Ljubljana] (IJS), Department of Theoretical Physics [Graz], Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche]-Karl-Franzens-Universität [Graz, Autriche], Laboratoire de Physique de la Matière Condensée (LPMC), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], Physics, Strongly Correlated Electrons (cond-mat.str-el), biology, Condensed matter physics, FOS: Physical sciences, Angle-resolved photoemission spectroscopy, Fermi energy, Condensed Matter Physics, biology.organism_classification, 01 natural sciences, 010305 fluids & plasmas, Electronic, Optical and Magnetic Materials, Renormalization, Condensed Matter - Strongly Correlated Electrons, Dynamical mean field theory, 0103 physical sciences, Dispersion (optics), Quasiparticle, Lanio, Condensed Matter::Strongly Correlated Electrons, Strongly correlated material, Atomic physics, 010306 general physics, ComputingMilieux_MISCELLANEOUS
Abstract: Recent angular-resolved photoemission experiments on LaNiO$_3$ reported a renormalization of the Fermi velocity of $e_g$ quasiparticles, a kink in their dispersion at $ -0.2$ eV and a large broadening and weakened dispersion of the occupied $t_{2g}$ states. We show here that all these features result from electronic correlations and are quantitatively reproduced by calculations combining density-functional theory and dynamical mean-field theory. The importance and general relevance of correlation effects in filled bands coupled by inter-orbital interactions to a partially-filled band are pointed out., Comment: 5 pages, 5 figures
Published: 2012
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21. Geophysical and atmospheric evolution of habitable planets

Author: Günter Stangl, Glenn J. White, Thomas Henning, Doris Breuer, W. Hausleitner, Helfried K. Biernat, Jean-Mathias Grießmeier, Andreas Quirrenbach, Jonathan I. Lunine, Hannes Gröller, Eric Chassefière, Tom Herbst, Charles Beichman, Yuri N. Kulikov, Richard Lundin, Alan J. Penny, Herbert Lichtenegger, René Liseau, Uwe Motschmann, Helmut Lammer, Carlos Eiroa, Lisa Kaltenegger, Francesco Paresce, Tilman Spohn, Petra Odert, John Parnell, François Leblanc, Heike Rauer, Nikolai V. Erkaev, Esa Kallio, A. Stadelmann, Jean Schneider, Huub Röttgering, Martin Leitzinger, Maxim L. Khodachenko, Alain Léger, Arnold Hanslmeier, Giovanna Tinetti, Siegfried J. Bauer, William C. Danchi, Frances Westall, Malcolm Fridlund, Daphne Stam, Franck Selsis, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), PLANETO - 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), 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), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Netherlands Institute for Radio Astronomy (ASTRON), Polar Geophysical Institute of Russian Academy of Sciences (PGI), Russian Academy of Sciences [Moscow] (RAS), Institute of Computational Modelling of the Russian Academy of Sciences (ICM SB RAS), Siberian Branch of the Russian Academy of Sciences (SB RAS), Finnish Meteorological Institute (FMI), Swedish Institute of Space Physics [Kiruna] (IRF), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche], NASA ExoPlanet Science Institute (NExScI), California Institute of Technology (CALTECH), NASA Goddard Space Flight Center (GSFC), Universidad Autonoma de Madrid (UAM), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institut d'astrophysique spatiale (IAS), Department of Radio and Space Science [Göteborg], Chalmers University of Technology [Göteborg], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Institut für Theoretische Physik [Braunschweig], Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Istituto Nazionale di Astrofisica (INAF), Department of Geology and Petroleum Geology [Aberdeen], University of Aberdeen, STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg], Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), University College of London [London] (UCL), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Karl-Franzens-Universität Graz, Universidad Autónoma de Madrid (UAM), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Harvard University-Smithsonian Institution, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Universität Heidelberg [Heidelberg] = Heidelberg University, and Universiteit Leiden
Subjects: 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Kepler-69c, Habitability, Rare Earth hypothesis, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Planets, Environment, 01 natural sciences, Astrobiology, Physics::Geophysics, Eccentric Jupiter, Magnetics, Galactic habitable zone, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Terrestrial planets, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Radiation, Planetary habitability, Atmosphere, Astronomy, Water, Geophysics, Agricultural and Biological Sciences (miscellaneous), Habitability of orange dwarf systems, Earth analog, 13. Climate action, Space and Planetary Science, Atmosphere evolution, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Evolution, Planetary, Geology
Abstract: International audience; The evolution of Earth-like habitable planets is a complex process that depends on the geodynamical and geophysical environments. In particular, it is necessary that plate tectonics remain active over billions of years. These geophysically active environments are strongly coupled to a planet's host star parameters, such as mass, luminosity and activity, orbit location of the habitable zone, and the planet's initial water inventory. Depending on the host star's radiation and particle flux evolution, the composition in the thermosphere, and the availability of an active magnetic dynamo, the atmospheres of Earth-like planets within their habitable zones are differently affected due to thermal and nonthermal escape processes. For some planets, strong atmospheric escape could even effect the stability of the atmosphere
Published: 2010
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22. Decrease of VLF transmitter signal and Chorus-whistler waves before l'Aquila earthquake occurrence

Author: Patrick H. M. Galopeau, W. Voller, R. Döller, Mohammed Y. Boudjada, Iren Adelina Moldovan, Maria Solovieva, Konrad Schwingenschuh, P. F. Biagi, M. Ampferer, O. A. Molchanov, Michel Parrot, Helfried K. Biernat, G. Stangl, Helmut Lammer, A. Rohznoi, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Institute for Geophysics, Astrophysics and Meteorology [Graz] (IGAM), Karl-Franzens-Universität Graz, Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Physics [Bari], Università degli studi di Bari Aldo Moro = University of Bari Aldo Moro (UNIBA), HELIOS - 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), Department of Theoretical Physics [Graz], Institute of Physics [Graz], Karl-Franzens-Universität Graz-Karl-Franzens-Universität Graz, Federal Office of Metrology and Surveying [Vienna] (BEV), National Institute for Earth Physics [Romania] - Institutul Național pentru Fizica Pământului (NIEP), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Università degli studi di Bari Aldo Moro (UNIBA), Karl-Franzens-Universität [Graz, Autriche]-Karl-Franzens-Universität [Graz, Autriche], and National Institute for Earth Physics [Bucharest] (NIEP)
Subjects: 010504 meteorology & atmospheric sciences, Whistler, 0211 other engineering and technologies, 02 engineering and technology, 01 natural sciences, Signal, lcsh:TD1-1066, lcsh:Environmental technology. Sanitary engineering, lcsh:Environmental sciences, 0105 earth and related environmental sciences, lcsh:GE1-350, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], 021110 strategic, defence & security studies, biology, lcsh:QE1-996.5, Transmitter, lcsh:Geography. Anthropology. Recreation, Chorus, Spectral density, biology.organism_classification, Intensity (physics), lcsh:Geology, Earth's magnetic field, lcsh:G, 13. Climate action, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Ionosphere, Geology, Seismology
Abstract: We investigate the VLF emissions observed by the Instrument Champ Electrique (ICE) experiment onboard the DEMETER micro-satellite. We analyze intensity level variation 10 days before and after the occurrence of l'Aquila earthquake (EQ). We found a clear decrease of the VLF received signal related to ionospheric whistler mode (mainly Chorus emission) and to signal transmitted by the DFY VLF station in Germany, few days (more than one week) before the earthquake. The VLF power spectral density decreases of more than two orders of magnitude until the EQ, and it recovers to normal levels just after the EQ occurrence. The geomagnetic activity is principally weak four days before EQ and increases again one day before l'Aquila seismic event. Our results are discussed in the frame of short- and long-terms earthquakes prediction focusing on the crucial role of the magnetic field of the Earth.
Published: 2010
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23. Dynamical mean-field theory within an augmented plane-wave framework: Assessing electronic correlations in the iron pnictide LaFeAsO

Author: Markus Aichhorn, Silke Biermann, Olivier Parcollet, Michel Ferrero, Leonid Pourovskii, Antoine Georges, Verónica Vildosola, Takashi Miyake, Department of Theoretical Physics [Graz], Institute of Physics [Graz], Karl-Franzens-Universität [Graz, Autriche]-Karl-Franzens-Universität [Graz, Autriche], Centre de Physique Théorique [Palaiseau] (CPHT), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Nanosystem Research Institute (NRI) RICS, AIST, Nanosystem Research Institute, Chaire Physique de la matière condensée (A. Georges), Collège de France (CdF (institution)), Laboratoire de Physique de la Matière Condensée (LPMC), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Japan Science and Technology Agency (JST), Karl-Franzens-Universität Graz-Karl-Franzens-Universität Graz, École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Collège de France - Chaire Physique de la matière condensée (A. Georges)
Subjects: Quantum Monte Carlo, Plane wave, FOS: Physical sciences, 02 engineering and technology, 01 natural sciences, Renormalization, Superconductivity (cond-mat.supr-con), Condensed Matter - Strongly Correlated Electrons, Atomic orbital, Quantum mechanics, 0103 physical sciences, Sensitivity (control systems), 010306 general physics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Wannier function, Degree (graph theory), Strongly Correlated Electrons (cond-mat.str-el), Condensed Matter - Superconductivity, 021001 nanoscience & nanotechnology, Condensed Matter Physics, Coupling (probability), Electronic, Optical and Magnetic Materials, Condensed Matter::Strongly Correlated Electrons, 0210 nano-technology
Abstract: We present an approach that combines the local density approximation (LDA) and the dynamical mean-field theory (DMFT) in the framework of the full-potential linear augmented plane waves (FLAPW) method. Wannier-like functions for the correlated shell are constructed by projecting local orbitals onto a set of Bloch eigenstates located within a certain energy window. The screened Coulomb interaction and Hund's coupling are calculated from a first-principle constrained RPA scheme. We apply this LDA+DMFT implementation, in conjunction with continuous-time quantum Monte-Carlo, to study the electronic correlations in LaFeAsO. Our findings support the physical picture of a metal with intermediate correlations. The average value of the mass renormalization of the Fe 3d bands is about 1.6, in reasonable agreement with the picture inferred from photoemission experiments. The discrepancies between different LDA+DMFT calculations (all technically correct) which have been reported in the literature are shown to have two causes: i) the specific value of the interaction parameters used in these calculations and ii) the degree of localization of the Wannier orbitals chosen to represent the Fe 3d states, to which many-body terms are applied. The latter is a fundamental issue in the application of many-body calculations, such as DMFT, in a realistic setting. We provide strong evidence that the DMFT approximation is more accurate and more straightforward to implement when well-localized orbitals are constructed from a large energy window encompassing Fe-3d, As-4p and O-2p, and point out several difficulties associated with the use of extended Wannier functions associated with the low-energy iron bands. Some of these issues have important physical consequences, regarding in particular the sensitivity to the Hund's coupling., Comment: 16 pages, 9 figures, published version
Published: 2009
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23 results on '"Institute of Physics [Graz]"'

1. Cometary Dust

2. Investigating Mercury's Environment with the Two-Spacecraft BepiColombo Mission

3. Characteristics of Resonant Electrons Interacting With Whistler Waves in the Nearest Dipolarizing Magnetotail

4. STIX X-ray microflare observations during the Solar Orbiter commissioning phase

5. How Dark Are Radial Breathing Modes in Plasmonic Nanodisks?

6. Dust of comet 67P/Churyumov-Gerasimenko collected by Rosetta/MIDAS: classification and extension to the nanometer scale

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9. Coulomb correlations in 4d and 5d oxides from first principles—or how spin–orbit materials choose their effective orbital degeneracies

10. How MIDAS improved our understanding of micrometre- sized cometary dust

11. The 2016 Feb 19 outburst of comet 67P/CG: an ESA Rosetta multi-instrument study

12. Aggregate dust particles at comet 67P/Churyumov–Gerasimenko

13. TRIQS/DFTTools: A TRIQS application for ab initio calculations of correlated materials

14. Similar behaviors of natural ELF/VLF ionospheric emissions and transmitter signals over seismic Adriatic regions

15. Fractal cometary dust – a window into the early Solar System

16. The PAC2MAN mission: a new tool to understand and predict solar energetic events

17. Solar Energetic Particles and Associated EIT Disturbances in Solar Cycle 23

18. Initiation of Coronal Mass Ejections by Sunspot Rotation

19. Edge scattering of surface plasmons excited by scanning tunneling microscopy

20. Hallmark of strong electronic correlations in LaNiO3: Photoemission kink and broadening of fully occupied bands

21. Geophysical and atmospheric evolution of habitable planets

22. Decrease of VLF transmitter signal and Chorus-whistler waves before l'Aquila earthquake occurrence

23. Dynamical mean-field theory within an augmented plane-wave framework: Assessing electronic correlations in the iron pnictide LaFeAsO

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23 results on '"Institute of Physics [Graz]"'

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