Solar wind energy flux observations in the inner heliosphere: first results from Parker Solar Probe

被引：12

作者：

Liu, M. ^{[1
]}

Issautier, K. ^{[1
]}

Meyer-Vernet, N. ^{[1
]}

Moncuquet, M. ^{[1
]}

Maksimovic, M. ^{[1
]}

Halekas, J. S. ^{[2
]}

Huang, J. ^{[3
]}

Griton, L. ^{[4
]}

Bale, S. ^{[5
,6
,7
,8
]}

Bonnell, J. W. ^{[5
]}

Case, A. W. ^{[9
]}

Goetz, K. ^{[10
]}

Harvey, P. R. ^{[5
]}

Kasper, J. C. ^{[3
,9
]}

MacDowall, R. J. ^{[11
]}

Malaspina, D. M. ^{[12
]}

Pulupa, M. ^{[5
]}

Stevens, M. L. ^{[9
]}

机构：

[1] Univ Paris, Sorbonne Univ, LESIA, Observ Paris,Univ PSL,CNRS, 5 Pl Jules Janssen, F-92195 Meudon, France

[2] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA

[3] Univ Michigan, Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA

[4] Univ Paul Sabatier, IRAP, 9 Av Colonel Roche,BP 4346, F-31028 Toulouse 4, France

[5] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[6] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[7] Imperial Coll London, Blackett Lab, London SW7 2AZ, England

[8] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England

[9] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA

[10] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[11] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Code 916, Greenbelt, MD 20771 USA

[12] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 650卷

关键词：

solar wind; Sun; heliosphere; corona; fundamental parameters; plasmas; acceleration of particles; QUASI-THERMAL NOISE; HELIUM ABUNDANCE; ELECTRON PARAMETERS; GLOBAL HELIOSPHERE; ALPHA-PARTICLE; SPEED; SPECTROSCOPY; TEMPERATURE; EVOLUTION; DENSITY;

D O I：

10.1051/0004-6361/202039615

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. We investigate the solar wind energy flux in the inner heliosphere using 12-day observations around each perihelion of Encounter One (E01), Two (E02), Four (E04), and Five (E05) of Parker Solar Probe (PSP), respectively, with a minimum heliocentric distance of 27.8 solar radii (R-circle dot). Methods. Energy flux was calculated based on electron parameters (density n(e), core electron temperature T-c, and suprathermal electron temperature T-h) obtained from the simplified analysis of the plasma quasi-thermal noise (QTN) spectrum measured by RFS/FIELDS and the bulk proton parameters (bulk speed V-p and temperature T-p) measured by the Faraday Cup onboard PSP, SPC/SWEAP. Results. Combining observations from E01, E02, E04, and E05, the averaged energy flux value normalized to 1 R<INF>circle dot</INF> plus the energy necessary to overcome the solar gravitation (W<INF>R<INF>circle dot</INF></INF>) is about 70 +/- 14 W m-2, which is similar to the average value (79 +/- 18 W m-2) derived by Le Chat, G., Issautier, K., & Meyer-Vernet, N. (2012, Sol. Phys., 279, 197) from 24-yr observations by Helios, Ulysses, and Wind at various distances and heliolatitudes. It is remarkable that the distributions of W<INF>R<INF>circle dot</INF></INF> are nearly symmetrical and well fitted by Gaussians, much more so than at 1 AU, which may imply that the small heliocentric distance limits the interactions with transient plasma structures.

引用

页数：7

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