Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh43a..03h&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #SH43A-03
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields, 7529 Photosphere
Scientific paper
The flux tube expansion (FTE) factor is a good proxy representing the solar coronal magnetic field, and it is widely used to infer the solar wind flow speed in the interplanetary space. In most cases, the FTE is assumed to be always greater than 1. However, for example, when the two strong magnetic field regions locate in a coronal hole, the flux tube from the region between them will be pressed due to the gradient of the magnetic field pressure. Therefore, the FTE can be less than 1. We performed the three-dimensional time-dependent MHD simulation of the solar corona and found that the plasma parameters in the regions with FTE less than 1 are similar to that in the plasma sheet; the density is higher and the plasma flow is slower than in the neighboring normal open field regions. Thus, the relationship between FTE and solar wind speed is not monotonic. We will show the simulated plasma properties and the obtained relationships between the magnetic field and the plasma in the solar corona.
Hayashi Kumiko
Liu Ya-Ying
Zhao Xiaopeng
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