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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00008008naa a2200757 4500
001oai:DiVA.org:uu-464260
003SwePub
008220119s2021 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-4642602 URI
0247 a https://doi.org/10.1051/0004-6361/2021410952 DOI
040 a (SwePub)uu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Louarn, P.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
2451 0a Multiscale views of an Alfvenic slow solar wind :b 3D velocity distribution functions observed by the Proton-Alpha Sensor of Solar Orbiter
264 c 2021-12-14
264 1b EDP Sciences,c 2021
338 a electronic2 rdacarrier
520 a Context. The Alfvenic slow solar wind is of particular interest, as it is often characterized by intense magnetic turbulence, complex proton 3D velocity distribution functions (VDF), and an ensuing richness of kinetic and dynamic processes.Aims. We take advantage of the fast time cadence of measurements taken by the Proton-Alpha Sensor (PAS) on board Solar Orbiter to analyze the kinetic properties of the proton population, the variability of their VDFs, and the possible link with propagating magnetic structures. We also study the magnetic (B) and velocity (V) correlation that characterizes this type of wind down to the ion gyroperiod.Methods. We analyzed the VDFs measured by PAS, a novelty that take advantages of the capability of 3D measurements at a 4 Hz cadence. In addition, we considered MAG observations.Results. We first show that there is a remarkable correlation between the B and V components observed down to timescales approaching the ion gyrofrequency. This concerns a wide variety of fluctuations, such as waves, isolated peaks, and discontinuities. The great variability of the proton VDFs is also documented. The juxtaposition of a core and a field-aligned beam is the norm but the relative density of the beam, drift speed, and temperatures can considerably change on scales as short as as a few seconds. The characteristics of the core are comparatively more stable. These variations in the beam characteristics mostly explain the variations in the total parallel temperature and, therefore, in the total anisotropy of the proton VDFs. Two magnetic structures that are associated with significant changes in the shape of VDFs, one corresponding to relaxation of total anisotropy and the other to its strong increase, are analyzed here. Our statistical analysis shows a clear link between total anisotropy (and, thus, beam characteristics) and the direction of B with respect to the Parker spiral. In the present case, flux tubes aligned with Parker spiral contain an average proton VDF with a much more developed beam (thus, with larger total anisotropy) than those that are inclined, perpendicular, or even reverse with regard to the outward direction.Conclusions. These observations document the variability of the proton VDF shape in relation to the propagation of magnetic structures. This is a key area of interest for understanding of the effect of turbulence on solar wind dynamics.
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
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
653 a solar wind
653 a turbulence
653 a plasmas
7001 a Fedorov, A.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Prech, L.u Charles Univ Prague, Fac Math & Phys, Dept Surface & Plasma Sci, Prague 18000 8, Czech Republic.4 aut
7001 a Owen, C. J.u Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.4 aut
7001 a Bruno, R.u INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy.4 aut
7001 a Livi, S.u Southwest Res Inst, 6220 Culebra Rd, San Antonio, TX 78238 USA.4 aut
7001 a Lavraud, B.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.;Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, Pessac, France.4 aut
7001 a Rouillard, A. P.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Genot, Vu Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Andre, N.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Fruit, G.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Reville, Vu Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Kieokaew, R.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Plotnikov, Iu Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Penou, E.u Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.4 aut
7001 a Barthe, A.u AKA, Toulouse, France.4 aut
7001 a Khataria, D.u Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.4 aut
7001 a Berthomier, M.u Ecole Polytech, Lab Phys Plasmas, Palaiseau, France.4 aut
7001 a D'Amicis, R.u INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy.4 aut
7001 a Sorriso-Valvo, Lucau Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen,Inst Sci & Technol Plasmas, Natl Res Council, Via Amendola 122-D, I-70126 Bari, Italy4 aut0 (Swepub:uu)lucso160
7001 a Allegrini, F.u Southwest Res Inst, 6220 Culebra Rd, San Antonio, TX 78238 USA.4 aut
7001 a Raines, J.u Univ Michigan, Dept Climate & Space Sci & Engn, Ann Harbour, MI USA.4 aut
7001 a Verscharen, D.u Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.;Univ New Hampshire, Space Sci Ctr, 8 Coll Rd, Durham, NH 03824 USA.4 aut
7001 a Fortunato, Vu Planetek Italia Srl, Via Massaua 12, I-70132 Bari, BA, Italy.4 aut
7001 a Mele, G.u Leonardo, Viale Lavoro 101, I-74123 Taranto, Italy.4 aut
7001 a Horbury, T. S.u Imperial Coll London, Blackett Lab, Space & Atmospher Phys, London SW7 2AZ, England.4 aut
7001 a O'brien, H.u Imperial Coll London, Blackett Lab, Space & Atmospher Phys, London SW7 2AZ, England.4 aut
7001 a Evans, Vu Imperial Coll London, Blackett Lab, Space & Atmospher Phys, London SW7 2AZ, England.4 aut
7001 a Angelini, Vu Imperial Coll London, Blackett Lab, Space & Atmospher Phys, London SW7 2AZ, England.4 aut
7001 a Maksimovic, M.u Univ PSL, Sorbonne Univ, Univ Paris, Observ Paris,LESIA,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France.4 aut
7001 a Kasper, J. C.u Univ Michigan, Dept Climate & Space Sci & Engn, Ann Harbour, MI USA.4 aut
7001 a Bale, S. D.u Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.4 aut
7102 a Univ Toulouse, Inst Rech Astrophys & Planetol, CNRS, CNES, Toulouse, France.b Charles Univ Prague, Fac Math & Phys, Dept Surface & Plasma Sci, Prague 18000 8, Czech Republic.4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 656q 656x 0004-6361x 1432-0746
8564 u https://doi.org/10.1051/0004-6361/202141095y Fulltext
8564 u https://uu.diva-portal.org/smash/get/diva2:1630157/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 u https://www.aanda.org/articles/aa/pdf/2021/12/aa41095-21.pdf
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-464260
8564 8u https://doi.org/10.1051/0004-6361/202141095

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