Solar corona magnetic structure and stagnated wind outflow

Solar observations made with the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliosphere Observatory (SoHO) spacecraft, have revealed that coronal protons and heavier ions have anisotropic temperature distributions. In a recent work we developed semi-empirical models for the sol...

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Detalles Bibliográficos
Publicado: 2005
Materias:
Corona
Solar wind plasma
Streamers
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p582_Vasquez
http://hdl.handle.net/20.500.12110/paper_0094243X_v784_n_p582_Vasquez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0094243X_v784_n_p582_Vasquez
record_format dspace
spelling paper:paper_0094243X_v784_n_p582_Vasquez2023-06-08T15:09:16Z Solar corona magnetic structure and stagnated wind outflow Corona Solar wind plasma Streamers Solar observations made with the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliosphere Observatory (SoHO) spacecraft, have revealed that coronal protons and heavier ions have anisotropic temperature distributions. In a recent work we developed semi-empirical models for the solar minimum corona to investigate the effect of the observed proton anisotropy on the coronal magnetic structure and the bimodal solar wind. Here we highlight the effect that the resulting particular geometry of the magnetic field around the streamer belt has on the solar wind. The open magnetic field lines surrounding the streamer belt (streamer legs) have non-monotonic expansion factors. This feature produces a stagnated outflow around the streamer magnetic cusp point, located at the top of the streamer belt closed magnetic field lines (streamer core). We find that this flow stagnation effect extends over quite important distances (of order 1R⊙) from the streamer cusp location. © 2005 American Institute of Physics. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p582_Vasquez http://hdl.handle.net/20.500.12110/paper_0094243X_v784_n_p582_Vasquez
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Corona
Solar wind plasma
Streamers
spellingShingle Corona
Solar wind plasma
Streamers
Solar corona magnetic structure and stagnated wind outflow
topic_facet Corona
Solar wind plasma
Streamers
description Solar observations made with the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliosphere Observatory (SoHO) spacecraft, have revealed that coronal protons and heavier ions have anisotropic temperature distributions. In a recent work we developed semi-empirical models for the solar minimum corona to investigate the effect of the observed proton anisotropy on the coronal magnetic structure and the bimodal solar wind. Here we highlight the effect that the resulting particular geometry of the magnetic field around the streamer belt has on the solar wind. The open magnetic field lines surrounding the streamer belt (streamer legs) have non-monotonic expansion factors. This feature produces a stagnated outflow around the streamer magnetic cusp point, located at the top of the streamer belt closed magnetic field lines (streamer core). We find that this flow stagnation effect extends over quite important distances (of order 1R⊙) from the streamer cusp location. © 2005 American Institute of Physics.
title Solar corona magnetic structure and stagnated wind outflow
title_short Solar corona magnetic structure and stagnated wind outflow
title_full Solar corona magnetic structure and stagnated wind outflow
title_fullStr Solar corona magnetic structure and stagnated wind outflow
title_full_unstemmed Solar corona magnetic structure and stagnated wind outflow
title_sort solar corona magnetic structure and stagnated wind outflow
publishDate 2005
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p582_Vasquez
http://hdl.handle.net/20.500.12110/paper_0094243X_v784_n_p582_Vasquez
_version_ 1768541744653139968

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