Modelling the magnetic field evolution with potential fields

Details Modelling the magnetic field evolution with potential fields Modelling the magnetic field evolution with potential fields

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43b1945r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43B-1945

Astronomy and Astrophysics

Astrophysics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

The potential field is a quite simple assumption to model the magnetic field of the solar corona as it relies only on the vertical component of the magnetic field measured on the photosphere. However, with the always increasing amount of line-of-sight magnetic field, this assumption is often the best way to approximate the corona magnetic field and to derive useful information on its time evolution. We use SDO/HMI and Hinode/SOT data to study the evolution of quiet-Sun regions and active regions. We focus our study on the magnetic topology of the magnetic configurations, and on the energy budget. We show that the magnetic topology of potential fields is consistent with the observed EUV intensity as observed by SDO/AIA. A quantitative comparison between the EUV emission and magnetic energy density is provided: the relationship between EUV brightenings and magnetic topology is statistically difficult to establish. We also investigate the evolution of the magnetic energy of the potential field related to the activity of the region: the emerging magnetic field and the separation between polarities are mainly responsible for the fluctuation of the magnetic energy budget.

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