Open AccessThree‐dimensional MHD modeling of the global corona throughout solar cycle 23
Author(s) -
Hu Y. Q.,
Feng X. S.,
Wu S. T.,
Song W. B.
Publication year - 2008
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2007ja012750
Subject(s) - magnetohydrodynamics , physics , coronal mass ejection , corona (planetary geology) , coronal hole , nanoflares , interplanetary magnetic field , current sheet , coronal loop , heliospheric current sheet , helmet streamer , solar wind , computational physics , astronomy , magnetic field , astrobiology , quantum mechanics , venus
Based on the space‐time conservation element and solution element (CESE) method, we have recently developed a novel 3D magnetohydrodynamic (MHD) model for the solar corona and interplanetary study. Our aim here is to describe the application of this new MHD model to study the global coronal magnetic structures by using the observed line‐of‐sight photospheric magnetic field from the Wilcox Solar Observatory (WSO) as boundary conditions. With this model, the magnetic structures of the global corona are obtained for fifteen Carrington Rotations (CRs) spanning solar cycle 23. The results illustrate how the shape and location of the heliospheric current sheet (HCS) and the coronal magnetic field configuration evolve during the course of the solar cycle. Comparison between our numerical results for the coronal magnetic structures and those from the standard potential field source surface (PFSS) model, with, in addition, white‐light observations further validates this new MHD model. The source surface neutral lines calculated from the MHD and PFSS models generally match each other closely; however, differences occur at different phases in the solar cycle. The location of the HCS shows good overall agreement with the bright structures in the observed white‐light intensity pattern, especially around solar minimum or well after solar maximum, and this result confirms that the observed white‐light streamer structures originate from a single, large‐scale plasma sheet located near the HCS.