First polar observations of the fast solar wind with the Metis - Solar Orbiter coronagraph: Role of 2D turbulence energy dissipation in the wind acceleration

被引：9

作者：

Telloni, D. ^{[1
]}

Antonucci, E. ^{[1
]}

Adhikari, L. ^{[2
]}

Zank, G. P. ^{[2
,3
]}

Giordano, S. ^{[1
]}

Vai, M. ^{[1
]}

Zhao, L. -l. ^{[2
]}

Andretta, V. ^{[4
]}

Burtovoi, A. ^{[5
]}

Capuano, G. E. ^{[6
,7
]}

Da Deppo, V. ^{[8
]}

De Leo, Y. ^{[7
,9
]}

Fineschi, S. ^{[1
]}

Grimani, C. ^{[10
,11
]}

Heinzel, P. ^{[12
,13
]}

Jerse, G. ^{[14
]}

Landini, F. ^{[1
]}

Liberatore, A. ^{[15
]}

Moses, J. D. ^{[16
]}

Naletto, G. ^{[17
]}

Nicolini, G. ^{[1
]}

Pancrazzi, M. ^{[1
]}

Romoli, M. ^{[18
]}

Russano, G. ^{[4
]}

Sasso, C. ^{[4
]}

Slemer, A. ^{[8
]}

Spadaro, D. ^{[6
]}

Stangalini, M. ^{[19
]}

Susino, R. ^{[1
]}

Teriaca, L. ^{[9
]}

Uslenghi, M. ^{[20
]}

Sorriso-Valvo, L. ^{[21
,22
]}

Marino, R. ^{[23
]}

Perrone, D. ^{[19
]}

D'Amicis, R. ^{[24
]}

Bruno, R. ^{[24
]}

机构：

[1] Natl Inst Astrophys, Astrophys Observ Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy

[2] Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA

[3] Univ Alabama Huntsville, Dept Space Sci, Huntsville, AL 35805 USA

[4] Natl Inst Astrophys, Astron Observ Capodimonte, Sal Moiariello 16, I-80131 Naples, Italy

[5] Natl Inst Astrophys, Astrophys Observ Arcetri, Largo Enr Fermi 5, I-50125 Florence, Italy

[6] Natl Inst Astrophys, Astrophys Observ Catania, Via St Sofia 78, I-95123 Catania, Italy

[7] Univ Catania, Dept Phys & Astron, Via St Sofia 64, I-95123 Catania, Italy

[8] CNR, Inst Photon & Nanotechnol, Via Trasea 7, I-35131 Padua, Italy

[9] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany

[10] Univ Urbino Carlo Bo, Dept Pure & Appl Sci, Via St Chiara 27, I-61029 Urbino, Italy

[11] Natl Inst Nucl Phys, Sect Florence, Via Bruno Rossi 1, I-50019 Sesto Fiorentino, Italy

[12] Czech Acad Sci, Astron Inst, Fricova 298, Ondrejov 25165, Czech Republic

[13] Univ Wroclaw, Ctr Sci Excellence Solar & Stellar Act, ul Kopern 11, PL-51622 Wroclaw, Poland

[14] Natl Inst Astrophys, Astron Observ Trieste, Local Basovizza 302, I-34149 Trieste, Italy

[15] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[16] NASA, Washington, DC 20546 USA

[17] Univ Padua, Dept Phys & Astron, Via Francesco Marzolo 8, I-35131 Padua, Italy

[18] Univ Florence, Dept Phys & Astron, Via Giovanni Sansone 1, I-50019 Sesto Fiorentino, Italy

[19] Italian Space Agcy, Via Politecn snc, I-00133 Rome, Italy

[20] Natl Inst Astrophys, Inst Space Astrophys & Cosm Phys Milan, Via Alfonso Corti 12, I-20133 Milan, Italy

[21] Inst Sci & Technol Plasmas, Natl Res Council, Via Amendola 122 D, I-70126 Bari, Italy

[22] Swedish Inst Space Phys, Angstrom Lab, Lagerhyddsvagen 1, S-75121 Uppsala, Sweden

[23] Univ Lyon, Univ Claude Bernard Lyon 1, Ecole Cent Lyon, Inst Natl Sci Appl Lyon, F-69134 Ecully, France

[24] Natl Inst Astrophys, Inst Space Astrophys & Planetol, Via Fosso Cavaliere 100, I-00133 Rome, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 670卷

关键词：

magnetohydrodynamics (MHD); Sun: corona; solar wind; Sun: UV radiation; MAGNETOHYDRODYNAMIC TURBULENCE; HOLE; DRIVEN; MODEL; TEMPERATURE; ANISOTROPY; VELOCITY; SPECTROMETER; HELIOSPHERE; TRANSPORT;

D O I：

10.1051/0004-6361/202245759

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The fast solar wind is known to emanate from polar coronal holes. Aims. This Letter reports the first estimate of the expansion rate of polar coronal flows performed by the Metis coronagraph on board Solar Orbiter. Methods. By exploiting simultaneous measurements in polarized white light and ultraviolet intensity of the neutral hydrogen Lyman-alpha line, it was possible to extend observations of the outflow velocity of the main component of the solar wind from polar coronal holes out to 5.5R(circle dot), the limit of diagnostic applicability and observational capabilities. Results. We complement the results obtained with analogous polar observations performed with the UltraViolet Coronagraph Spectrometer on board the SOlar and Heliospheric Observatory during the previous full solar activity cycle, and find them to be satisfactorily reproduced by a magnetohydrodynamic turbulence model. Conclusions. This suggests that the dissipation of 2D turbulence energy is a viable mechanism for coronal plasma heating and the subsequent acceleration of the fast solar wind.

引用

页数：6

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