Comparison of coronal extrapolation methods for cycle 24 using HMI data

Article


Arden, William, Norton, Aimee, Sun, Xudong and Zhao, Xuepu. 2016. "Comparison of coronal extrapolation methods for cycle 24 using HMI data." The Astrophysical Journal: an international review of astronomy and astronomical physics. 823 (1). https://doi.org/10.3847/0004-637X/823/1/21
Article Title

Comparison of coronal extrapolation methods for cycle 24 using HMI data

ERA Journal ID1057
Article CategoryArticle
AuthorsArden, William (Author), Norton, Aimee (Author), Sun, Xudong (Author) and Zhao, Xuepu (Author)
Journal TitleThe Astrophysical Journal: an international review of astronomy and astronomical physics
Journal Citation823 (1)
Article Number21
Number of Pages7
Year2016
PublisherIOP Publishing
Place of PublicationUnited States
ISSN0004-637X
1538-4357
Digital Object Identifier (DOI)https://doi.org/10.3847/0004-637X/823/1/21
Web Address (URL)https://iopscience.iop.org/article/10.3847/0004-637X/823/1/21
Abstract

Two extrapolation models of the solar coronal magnetic field are compared using magnetogram data from the Solar Dynamics Observatory/Helioseismic and Magnetic Imager instrument. The two models, a horizontal current-current sheet-source surface (HCCSSS) model and a potential field-source surface (PFSS) model, differ in their treatment of coronal currents. Each model has its own critical variable, respectively, the radius of a cusp surface and a source surface, and it is found that adjusting these heights over the period studied allows for a better fit between the models and the solar open flux at 1 au as calculated from the Interplanetary Magnetic Field (IMF). The HCCSSS model provides the better fit for the overall period from 2010 November to 2015 May as well as for two subsets of the period: the minimum/rising part of the solar cycle and the recently identified peak in the IMF from mid-2014 to mid-2015 just after solar maximum. It is found that an HCCSSS cusp surface height of 1.7 R o provides the best fit to the IMF for the overall period, while 1.7 and 1.9 R o give the best fits for the two subsets. The corresponding values for the PFSS source surface height are 2.1, 2.2, and 2.0 R o respectively. This means that the HCCSSS cusp surface rises as the solar cycle progresses while the PFSS source surface falls.

Keywordssolar cycle, solar corona
Contains Sensitive ContentDoes not contain sensitive content
ANZSRC Field of Research 2020519999. Other physical sciences not elsewhere classified
Public Notes

File reproduced in accordance with the copyright policy of the publisher/author.

Byline AffiliationsSchool of Agricultural, Computational and Environmental Sciences
Stanford University, United States
Institution of OriginUniversity of Southern Queensland
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