Validation of two MHD models of the solar corona with rotational tomography

We demonstrate a validation of two 3D MHD models of the corona by comparing density values from solar rotational tomography (SRT) to densities and morphological properties of the two MHD solutions for CR 2029 (2005 April 21-May 18). The two MHD models are given by the Stanford and Michigan models, a...

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Autores principales: Vasquez, A.M., Frazin, R.A., Hayashi, K., Sokolov, I.V., Cohen, O., Manchester IV, W.B., Kamalabadi, F.
Formato: JOUR
Materias:
Methods: numerical
Solar wind
Sun: corona
Sun: magnetic fields
Techniques: image processing
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_0004637X_v682_n2_p1328_Vasquez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_0004637X_v682_n2_p1328_Vasquez
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spelling todo:paper_0004637X_v682_n2_p1328_Vasquez2023-10-03T14:02:09Z Validation of two MHD models of the solar corona with rotational tomography Vasquez, A.M. Frazin, R.A. Hayashi, K. Sokolov, I.V. Cohen, O. Manchester IV, W.B. Kamalabadi, F. Methods: numerical Solar wind Sun: corona Sun: magnetic fields Techniques: image processing We demonstrate a validation of two 3D MHD models of the corona by comparing density values from solar rotational tomography (SRT) to densities and morphological properties of the two MHD solutions for CR 2029 (2005 April 21-May 18). The two MHD models are given by the Stanford and Michigan models, and both use the same synoptic magnetogram from MDI as a lower boundary condition. The SRT reconstructions are based on polarized white-light images MLSO Mk IV data for the region between 1.1 and 1.5 R ⊙ (solar radii) and LASCO C2 for the region between 2.3 and 6.0 R ⊙ . While the Stanford MHD model reasonably reproduces the tomographic density over the south pole, it fares less well over the north pole, and the Michigan MHD model underestimates the density over both poles. At lower latitudes, we find that while the MHD models have better agreement with the tomographic densities in the region below 3.5 R ⊙ at larger heights the agreement is more problematic. Our interpretation is that the base densities and temperatures of the models need to be improved, as well as their radial density gradients. © 2008. The American Astronomical Society. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_0004637X_v682_n2_p1328_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 Methods: numerical
Solar wind
Sun: corona
Sun: magnetic fields
Techniques: image processing
spellingShingle Methods: numerical
Solar wind
Sun: corona
Sun: magnetic fields
Techniques: image processing
Vasquez, A.M.
Frazin, R.A.
Hayashi, K.
Sokolov, I.V.
Cohen, O.
Manchester IV, W.B.
Kamalabadi, F.
Validation of two MHD models of the solar corona with rotational tomography
topic_facet Methods: numerical
Solar wind
Sun: corona
Sun: magnetic fields
Techniques: image processing
description We demonstrate a validation of two 3D MHD models of the corona by comparing density values from solar rotational tomography (SRT) to densities and morphological properties of the two MHD solutions for CR 2029 (2005 April 21-May 18). The two MHD models are given by the Stanford and Michigan models, and both use the same synoptic magnetogram from MDI as a lower boundary condition. The SRT reconstructions are based on polarized white-light images MLSO Mk IV data for the region between 1.1 and 1.5 R ⊙ (solar radii) and LASCO C2 for the region between 2.3 and 6.0 R ⊙ . While the Stanford MHD model reasonably reproduces the tomographic density over the south pole, it fares less well over the north pole, and the Michigan MHD model underestimates the density over both poles. At lower latitudes, we find that while the MHD models have better agreement with the tomographic densities in the region below 3.5 R ⊙ at larger heights the agreement is more problematic. Our interpretation is that the base densities and temperatures of the models need to be improved, as well as their radial density gradients. © 2008. The American Astronomical Society. All rights reserved.
format JOUR
author Vasquez, A.M.
Frazin, R.A.
Hayashi, K.
Sokolov, I.V.
Cohen, O.
Manchester IV, W.B.
Kamalabadi, F.
author_facet Vasquez, A.M.
Frazin, R.A.
Hayashi, K.
Sokolov, I.V.
Cohen, O.
Manchester IV, W.B.
Kamalabadi, F.
author_sort Vasquez, A.M.
title Validation of two MHD models of the solar corona with rotational tomography
title_short Validation of two MHD models of the solar corona with rotational tomography
title_full Validation of two MHD models of the solar corona with rotational tomography
title_fullStr Validation of two MHD models of the solar corona with rotational tomography
title_full_unstemmed Validation of two MHD models of the solar corona with rotational tomography
title_sort validation of two mhd models of the solar corona with rotational tomography
url http://hdl.handle.net/20.500.12110/paper_0004637X_v682_n2_p1328_Vasquez
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AT sokoloviv validationoftwomhdmodelsofthesolarcoronawithrotationaltomography
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