Flows in the solar atmosphere due to the eruptions on the 15th July, 2002

Which kind of flows are present during flares? Are they compatible with the present understanding of energy release and which model best describes the observations? We analyze successive flare events in order to answer these questions. The flares were observed in the magnetically complex NOAA active...

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Publicado:	2005
Materias:	Sun: corona Sun: coronal mass ejections (CMEs) Sun: flares Sun: UV radiation Cameras Charge coupled devices Cooling Electromagnetic wave emission Evaporation Extraterrestrial atmospheres Mathematical models Plasmas Spectrometers Sun Ultraviolet radiation Corona-Sun Coronal mass ejections (CMEs) Flares-Sun UV radiation-Sun Solar energy
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v438_n3_p1099_Harra http://hdl.handle.net/20.500.12110/paper_00046361_v438_n3_p1099_Harra
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046361_v438_n3_p1099_Harra
record_format	dspace
spelling	paper:paper_00046361_v438_n3_p1099_Harra2023-06-08T14:27:38Z Flows in the solar atmosphere due to the eruptions on the 15th July, 2002 Sun: corona Sun: coronal mass ejections (CMEs) Sun: flares Sun: UV radiation Cameras Charge coupled devices Cooling Electromagnetic wave emission Evaporation Extraterrestrial atmospheres Mathematical models Plasmas Spectrometers Sun Ultraviolet radiation Corona-Sun Coronal mass ejections (CMEs) Flares-Sun UV radiation-Sun Solar energy Which kind of flows are present during flares? Are they compatible with the present understanding of energy release and which model best describes the observations? We analyze successive flare events in order to answer these questions. The flares were observed in the magnetically complex NOAA active region (AR) 10030 on 15 July 2002. One of them is of GOES X-class. The description of these flares and how they relate to the break-out model is presented in Gary & Moore (2004). The Coronal Diagnostic Spectrometer on board SOHO observed this active region for around 14 h. The observed emission lines provided data from the transition region to the corona with a field of view covering more than half of the active region. In this paper we analyse the spatially resolved flows seen in the atmosphere from the preflare to the flare stages. We find evidence for evaporation occurring before the impulsive phase. During the main phase, the ongoing magnetic reconnection is demonstrated by upflows located at the edges of the flare loops (while downflows are found in the flare loops themselves). We also report the impact of a filament eruption on the atmosphere, with flows up to 300 km s-1 observed at transition-region temperatures in regions well away from the location of the pre-eruptive filament. Our results are consistent with the predictions of the break out model before the impulsive phase of the flare; while, as the flare progresses, the directions of the flows are consistent with flare models invoking evaporation followed by cooling and downward plasma motions in the flare loops. © ESO 2005. 2005 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v438_n3_p1099_Harra http://hdl.handle.net/20.500.12110/paper_00046361_v438_n3_p1099_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	Sun: corona Sun: coronal mass ejections (CMEs) Sun: flares Sun: UV radiation Cameras Charge coupled devices Cooling Electromagnetic wave emission Evaporation Extraterrestrial atmospheres Mathematical models Plasmas Spectrometers Sun Ultraviolet radiation Corona-Sun Coronal mass ejections (CMEs) Flares-Sun UV radiation-Sun Solar energy
spellingShingle	Sun: corona Sun: coronal mass ejections (CMEs) Sun: flares Sun: UV radiation Cameras Charge coupled devices Cooling Electromagnetic wave emission Evaporation Extraterrestrial atmospheres Mathematical models Plasmas Spectrometers Sun Ultraviolet radiation Corona-Sun Coronal mass ejections (CMEs) Flares-Sun UV radiation-Sun Solar energy Flows in the solar atmosphere due to the eruptions on the 15th July, 2002
topic_facet	Sun: corona Sun: coronal mass ejections (CMEs) Sun: flares Sun: UV radiation Cameras Charge coupled devices Cooling Electromagnetic wave emission Evaporation Extraterrestrial atmospheres Mathematical models Plasmas Spectrometers Sun Ultraviolet radiation Corona-Sun Coronal mass ejections (CMEs) Flares-Sun UV radiation-Sun Solar energy
description	Which kind of flows are present during flares? Are they compatible with the present understanding of energy release and which model best describes the observations? We analyze successive flare events in order to answer these questions. The flares were observed in the magnetically complex NOAA active region (AR) 10030 on 15 July 2002. One of them is of GOES X-class. The description of these flares and how they relate to the break-out model is presented in Gary & Moore (2004). The Coronal Diagnostic Spectrometer on board SOHO observed this active region for around 14 h. The observed emission lines provided data from the transition region to the corona with a field of view covering more than half of the active region. In this paper we analyse the spatially resolved flows seen in the atmosphere from the preflare to the flare stages. We find evidence for evaporation occurring before the impulsive phase. During the main phase, the ongoing magnetic reconnection is demonstrated by upflows located at the edges of the flare loops (while downflows are found in the flare loops themselves). We also report the impact of a filament eruption on the atmosphere, with flows up to 300 km s-1 observed at transition-region temperatures in regions well away from the location of the pre-eruptive filament. Our results are consistent with the predictions of the break out model before the impulsive phase of the flare; while, as the flare progresses, the directions of the flows are consistent with flare models invoking evaporation followed by cooling and downward plasma motions in the flare loops. © ESO 2005.
title	Flows in the solar atmosphere due to the eruptions on the 15th July, 2002
title_short	Flows in the solar atmosphere due to the eruptions on the 15th July, 2002
title_full	Flows in the solar atmosphere due to the eruptions on the 15th July, 2002
title_fullStr	Flows in the solar atmosphere due to the eruptions on the 15th July, 2002
title_full_unstemmed	Flows in the solar atmosphere due to the eruptions on the 15th July, 2002
title_sort	flows in the solar atmosphere due to the eruptions on the 15th july, 2002
publishDate	2005
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v438_n3_p1099_Harra http://hdl.handle.net/20.500.12110/paper_00046361_v438_n3_p1099_Harra
_version_	1768545626746781696

Flows in the solar atmosphere due to the eruptions on the 15th July, 2002

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