Calculating Non-Potentiality in Solar Active Regions Using SDO/HMI Vector Magnetic Field Data

Details Calculating Non-Potentiality in Solar Active Regions Using SDO/HMI Vector Magnetic Field Data Calculating Non-Potentiality in Solar Active Regions Using SDO/HMI Vector Magnetic Field Data

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11a1608b&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH11A-1608

Astronomy and Astrophysics

Astrophysics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere

Scientific paper

Non-potential magnetic fields in solar active regions are thought to be associated with flare occurrence. In this study, we parametrize the non-potentiality of several active regions, using data from the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory (SDO), and correlate these parameters with flare occurrence. In particular, we focus on a parameter that we call the Gradient-Weighted Inversion Line Length (GWILL). Using data from SOHO/MDI, Mason et al. found that GWILL generally tends to increase before a solar flare. We investigate whether extending the analysis of Mason et. al. to a three-dimensional field enables us to derive better near real-time indicators of flare occurrence. Before HMI, the availability of vector magnetograms was sparse at best. HMI provides continuous vector magnetogram data at a 12-minute cadence. As such, this study represents the first parametrization of non-potentiality in solar active regions using continuous vector magnetic field data.

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