The solar minimum corona from differential emission measure tomography

We present results derived from a dual-spacecraft tomographic reconstruction of the solar corona's three-dimensional (3D) extreme ultraviolet (EUV) emissivity. We use simultaneously taken STEREO A and B spacecraft EUVI images from Carrington rotation 2077 (UT 2008 November 20 06:56 through UT D...

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Guardado en:
Detalles Bibliográficos
Publicado: 2010
Materias:
Solar wind
Sun: activity
Sun: corona
Sun: magnetic topology
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v715_n2_p1352_Vasquez
http://hdl.handle.net/20.500.12110/paper_0004637X_v715_n2_p1352_Vasquez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v715_n2_p1352_Vasquez
record_format dspace
spelling paper:paper_0004637X_v715_n2_p1352_Vasquez2023-06-08T14:28:58Z The solar minimum corona from differential emission measure tomography Solar wind Sun: activity Sun: corona Sun: magnetic topology We present results derived from a dual-spacecraft tomographic reconstruction of the solar corona's three-dimensional (3D) extreme ultraviolet (EUV) emissivity. We use simultaneously taken STEREO A and B spacecraft EUVI images from Carrington rotation 2077 (UT 2008 November 20 06:56 through UT December 17 14:34). During this period, the spacecraft view angles were separated by an average 854 which allowed for the reconstruction to be performed with data gathered in about 3/4 of a full solar rotational time. The EUV reconstructions provide the 3D emissivity in each of the three EUVI Fe bands, in the range of heights 1.00-1.25R s. We use this information to perform local differential emission measure (LDEM) analysis. Taking moments of the so-derived LDEM distributions gives the 3D values of the electron density, temperature, and temperature spread. We determine relationships between the moments of the LDEM and the coronal magnetic field by making longitudinal averages of the moments, and relating them to the global-scale structures of a potential field source surface magnetic field model. In this way, we determine how the electron density, mean temperature, and temperature spread vary for different coronal structures. We draw conclusions about the relationship between the LDEM moments and the sources of the fast and slow solar winds, and the transition between the two regimes. © 2010. The American Astronomical Society. All rights reserved. 2010 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v715_n2_p1352_Vasquez http://hdl.handle.net/20.500.12110/paper_0004637X_v715_n2_p1352_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 Solar wind
Sun: activity
Sun: corona
Sun: magnetic topology
spellingShingle Solar wind
Sun: activity
Sun: corona
Sun: magnetic topology
The solar minimum corona from differential emission measure tomography
topic_facet Solar wind
Sun: activity
Sun: corona
Sun: magnetic topology
description We present results derived from a dual-spacecraft tomographic reconstruction of the solar corona's three-dimensional (3D) extreme ultraviolet (EUV) emissivity. We use simultaneously taken STEREO A and B spacecraft EUVI images from Carrington rotation 2077 (UT 2008 November 20 06:56 through UT December 17 14:34). During this period, the spacecraft view angles were separated by an average 854 which allowed for the reconstruction to be performed with data gathered in about 3/4 of a full solar rotational time. The EUV reconstructions provide the 3D emissivity in each of the three EUVI Fe bands, in the range of heights 1.00-1.25R s. We use this information to perform local differential emission measure (LDEM) analysis. Taking moments of the so-derived LDEM distributions gives the 3D values of the electron density, temperature, and temperature spread. We determine relationships between the moments of the LDEM and the coronal magnetic field by making longitudinal averages of the moments, and relating them to the global-scale structures of a potential field source surface magnetic field model. In this way, we determine how the electron density, mean temperature, and temperature spread vary for different coronal structures. We draw conclusions about the relationship between the LDEM moments and the sources of the fast and slow solar winds, and the transition between the two regimes. © 2010. The American Astronomical Society. All rights reserved.
title The solar minimum corona from differential emission measure tomography
title_short The solar minimum corona from differential emission measure tomography
title_full The solar minimum corona from differential emission measure tomography
title_fullStr The solar minimum corona from differential emission measure tomography
title_full_unstemmed The solar minimum corona from differential emission measure tomography
title_sort solar minimum corona from differential emission measure tomography
publishDate 2010
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v715_n2_p1352_Vasquez
http://hdl.handle.net/20.500.12110/paper_0004637X_v715_n2_p1352_Vasquez
_version_ 1768546282183327744

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