English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Slow wind belt in the quiet solar corona

Antonucci, E., Downs, C., Capuano, G. E., Spadaro, D., Susino, R., Telloni, D., et al. (2023). Slow wind belt in the quiet solar corona. Physics of Plasmas, 30, 022905. doi:10.1063/5.0132824.

Item is

Files

show Files

Locators

show
hide
Description:
-
OA-Status:
Not specified

Creators

show
hide
 Creators:
Antonucci, E., Author
Downs, C., Author
Capuano, G. E., Author
Spadaro, D., Author
Susino, R., Author
Telloni, D., Author
Andretta, V., Author
Da Deppo, V., Author
De Leo, Y.1, 2, Author           
Fineschi, S., Author
Frassetto, F., Author
Landini, F., Author
Naletto, G., Author
Nicolini, G., Author
Pancrazzi, M., Author
Romoli, M., Author
Stangalini, M., Author           
Teriaca, L.2, Author           
Uslenghi, M., Author
Affiliations:
1IMPRS for Solar System Science at the University of Göttingen, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832290              
2Department Sun and Heliosphere, Max Planck Institute for Solar System Research, Max Planck Society, ou_1832289              

Content

show
hide
Free keywords: Astrophysics - Solar and Stellar Astrophysics; Physics - Space Physics
 Abstract: The slow solar wind belt in the quiet corona, observed with the Metis coronagraph on board Solar Orbiter on May 15, 2020, during the activity minimum of the cycle 24, in a field of view extending from 3.8 R ⊙ to 7.0 R ⊙, is formed by a slow and dense wind stream running along the coronal current sheet, accelerating in the radial direction and reaching at 6.8 R ⊙ a speed within 150 and 190 km s-1, depending on the assumptions on the velocity distribution of the neutral hydrogen atoms in the coronal plasma. The slow stream is separated by thin regions of high velocity shear from faster streams, almost symmetric relative to the current sheet, with peak velocity within 175 and 230 km s-1 at the same coronal level. The density-velocity structure of the slow wind zone is discussed in terms of the expansion factor of the open magnetic field lines that is known to be related to the speed of the quasi-steady solar wind, and in relation to the presence of a web of quasi-separatrix layers, S-web, the potential sites of reconnection that release coronal plasma into the wind. The parameters characterizing the coronal magnetic field lines are derived from 3D MHD model calculations. The S-web is found to coincide with the latitudinal region where the slow wind is observed in the outer corona and is surrounded by thin layers of open field lines expanding in a non-monotonic way.

Details

show
hide
Language(s):
 Dates: 2023-02-01
 Publication Status: Issued
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: -
 Identifiers: DOI: 10.1063/5.0132824
ISSN: 1070-664X
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Physics of Plasmas
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 30 Sequence Number: - Start / End Page: 022905 Identifier: -