Outflows at the edges of active regions: Contribution to solar wind formation?

The formation of the slow solar wind has been debated for many years. In this Letter we show evidence of persistent outflow at the edges of an active region as measured by the EUV Imaging Spectrometer on board Hinode. The Doppler velocity ranged between 20 and 50 km s -1 and was consistent with a st...

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Detalles Bibliográficos
Publicado: 2008
Materias:
Solar wind
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v676_n2PART2_pL147_Harra
http://hdl.handle.net/20.500.12110/paper_0004637X_v676_n2PART2_pL147_Harra
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v676_n2PART2_pL147_Harra
record_format dspace
spelling paper:paper_0004637X_v676_n2PART2_pL147_Harra2023-06-08T14:28:54Z Outflows at the edges of active regions: Contribution to solar wind formation? Solar wind The formation of the slow solar wind has been debated for many years. In this Letter we show evidence of persistent outflow at the edges of an active region as measured by the EUV Imaging Spectrometer on board Hinode. The Doppler velocity ranged between 20 and 50 km s -1 and was consistent with a steady flow seen in the X-Ray Telescope. The latter showed steady, pulsing outflowing material and some transverse motions of the loops. We analyze the magnetic field around the active region and produce a coronal magnetic field model. We determine from, the latter that the outflow speeds adjusted for line-of-sight effects can reach over 100 km s -1 . We can interpret this outflow as expansion of loops that lie over the active region, which may either reconnect with neighboring large-scale loops or are likely to open to the interplanetary space. This material constitutes at least part of the slow solar wind. © 2008. The American Astronomical Society. All rights reserved. 2008 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v676_n2PART2_pL147_Harra http://hdl.handle.net/20.500.12110/paper_0004637X_v676_n2PART2_pL147_Harra
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Solar wind
spellingShingle Solar wind
Outflows at the edges of active regions: Contribution to solar wind formation?
topic_facet Solar wind
description The formation of the slow solar wind has been debated for many years. In this Letter we show evidence of persistent outflow at the edges of an active region as measured by the EUV Imaging Spectrometer on board Hinode. The Doppler velocity ranged between 20 and 50 km s -1 and was consistent with a steady flow seen in the X-Ray Telescope. The latter showed steady, pulsing outflowing material and some transverse motions of the loops. We analyze the magnetic field around the active region and produce a coronal magnetic field model. We determine from, the latter that the outflow speeds adjusted for line-of-sight effects can reach over 100 km s -1 . We can interpret this outflow as expansion of loops that lie over the active region, which may either reconnect with neighboring large-scale loops or are likely to open to the interplanetary space. This material constitutes at least part of the slow solar wind. © 2008. The American Astronomical Society. All rights reserved.
title Outflows at the edges of active regions: Contribution to solar wind formation?
title_short Outflows at the edges of active regions: Contribution to solar wind formation?
title_full Outflows at the edges of active regions: Contribution to solar wind formation?
title_fullStr Outflows at the edges of active regions: Contribution to solar wind formation?
title_full_unstemmed Outflows at the edges of active regions: Contribution to solar wind formation?
title_sort outflows at the edges of active regions: contribution to solar wind formation?
publishDate 2008
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v676_n2PART2_pL147_Harra
http://hdl.handle.net/20.500.12110/paper_0004637X_v676_n2PART2_pL147_Harra
_version_ 1768542061131202560

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