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Sökning: onr:"swepub:oai:DiVA.org:uu-464268" > Observations of whi...

LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00008211naa a2200817 4500
001oai:DiVA.org:uu-464268
003SwePub
008220119s2021 | |||||||||||000 ||eng|
009oai:DiVA.org:kth-307350
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-4642682 URI
0247 a https://doi.org/10.1051/0004-6361/2021409322 DOI
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-3073502 URI
040 a (SwePub)uud (SwePub)kth
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Chust, T.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
2451 0a Observations of whistler mode waves by Solar Orbiter's RPW Low Frequency Receiver (LFR) :b In-flight performance and first results
264 c 2021-12-14
264 1b EDP Sciences,c 2021
338 a electronic2 rdacarrier
500 a QC 20220124
520 a Context. The Radio and Plasma Waves (RPW) instrument is one of the four in situ instruments of the ESA/NASA Solar Orbiter mission, which was successfully launched on February 10, 2020. The Low Frequency Receiver (LFR) is one of its subsystems, designed to characterize the low frequency electric (quasi-DC - 10 kHz) and magnetic (similar to 1 Hz-10 kHz) fields that develop, propagate, interact, and dissipate in the solar wind plasma. Combined with observations of the particles and the DC magnetic field, LFR measurements will help to improve the understanding of the heating and acceleration processes at work during solar wind expansion.Aims. The capability of LFR to observe and analyze a variety of low frequency plasma waves can be demontrated by taking advantage of whistler mode wave observations made just after the near-Earth commissioning phase of Solar Orbiter. In particular, this is related to its capability of measuring the wave normal vector, the phase velocity, and the Poynting vector for determining the propagation characteristics of the waves.Methods. Several case studies of whistler mode waves are presented, using all possible LFR onboard digital processing products, waveforms, spectral matrices, and basic wave parameters.Results. Here, we show that whistler mode waves can be very properly identified and characterized, along with their Doppler-shifted frequency, based on the waveform capture as well as on the LFR onboard spectral analysis.Conclusions. Despite the fact that calibrations of the electric and magnetic data still require some improvement, these first whistler observations show a good overall consistency between the RPW LFR data, indicating that many science results on these waves, as well as on other plasma waves, can be obtained by Solar Orbiter in the solar wind.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
650 7a NATURVETENSKAPx Fysikx Fusion, plasma och rymdfysik0 (SwePub)103032 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Fusion, Plasma and Space Physics0 (SwePub)103032 hsv//eng
653 a solar wind
653 a waves
653 a plasmas
653 a instrumentation
653 a miscellaneous
7001 a Kretzschmar, M.u Univ Orleans, CNRS, LPC2E, 3A Ave Rech Sci, Orleans, France.4 aut
7001 a Graham, Daniel B.u Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)dangr618
7001 a Le Contel, O.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Retino, A.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Alexandrova, A.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.,Czech Acad Sci, Astron Inst, Prague, Czech Republic.;Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.4 aut
7001 a Berthomier, M.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Hadid, L. Z.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Sahraoui, F.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Jeandet, A.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Leroy, P.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Pellion, J-Cu Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Bouzid, Vu Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Katra, B.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Piberne, R.u Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.4 aut
7001 a Khotyaintsev, Yuri V.u Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen4 aut0 (Swepub:uu)ykh28990
7001 a Vaivads, Andrisu KTH,Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Royal Inst Technol, Sch Elect Engn & Comp Sci, Dept Space & Plasma Phys, Stockholm, Sweden.,Rymd- och plasmafysik,Swedish Inst Space Phys IRF, Uppsala, Sweden4 aut0 (Swepub:kth)u167dmzs
7001 a Krasnoselskikh, Vu Univ Orleans, CNRS, LPC2E, 3A Ave Rech Sci, Orleans, France.4 aut
7001 a Soucek, J.u Czech Acad Sci, Dept Space Phys, Inst Atmospher Phys, Prague, Czech Republic.4 aut
7001 a Santolik, O.u Czech Acad Sci, Dept Space Phys, Inst Atmospher Phys, Prague, Czech Republic.;Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.4 aut
7001 a Lorfevre, E.u CNES, 18 Ave Edouard Belin, F-31400 Toulouse, France.4 aut
7001 a Plettemeier, D.u Tech Univ Dresden, Wurzburger Str 35, D-01187 Dresden, Germany.4 aut
7001 a Steller, M.u Austrian Acad Sci, Space Res Inst, Graz, Austria.4 aut
7001 a Stverak, S.u Czech Acad Sci, Astron Inst, Prague, Czech Republic.,Univ PSL, Sorbonne Univ, Univ Paris, Observ Paris,LESIA,CNRS, Meudon, France.,Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.;Univ Calif Berkeley, Phys Dept, Berkeley, CA USA.;Stellar Sci, Berkeley, CA USA.4 aut
7001 a Vecchio, A.u Czech Acad Sci, Astron Inst, Prague, Czech Republic.;Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.,Imperial Coll, Dept Phys, London SW7 2AZ, England.4 aut
7001 a Maksimovic, M.u Univ PSL, Sorbonne Univ, Univ Paris, Observ Paris,LESIA,CNRS, Meudon, France.;Radboud Univ Nijmegen, Dept Astrophys, Radboud Radio Lab, Nijmegen, Netherlands.4 aut
7001 a Bale, S. D.u Univ PSL, Sorbonne Univ, Univ Paris, Observ Paris,LESIA,CNRS, Meudon, France.4 aut
7001 a Horbury, T. S.u Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.;Univ Calif Berkeley, Phys Dept, Berkeley, CA USA.;Stellar Sci, Berkeley, CA USA.4 aut
7001 a O'Brien, H.u Imperial Coll, Dept Phys, London SW7 2AZ, England.4 aut
7001 a Evans, Vu Imperial Coll, Dept Phys, London SW7 2AZ, England.4 aut
7001 a Angelini, Vu Imperial Coll, Dept Phys, London SW7 2AZ, England.4 aut
7102 a Sorbonne Univ, Univ Paris Saclay, Observ Paris, Ecole Polytech,LPP,CNRS, Paris, France.b Univ Orleans, CNRS, LPC2E, 3A Ave Rech Sci, Orleans, France.4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 656q 656x 0004-6361x 1432-0746
8564 u https://doi.org/10.1051/0004-6361/202140932y Fulltext
8564 u https://uu.diva-portal.org/smash/get/diva2:1630063/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 u https://www.aanda.org/articles/aa/pdf/2021/12/aa40932-21.pdf
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-464268
8564 8u https://doi.org/10.1051/0004-6361/202140932
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-307350

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