Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh13a1927l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH13A-1927
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields
Scientific paper
Solar active regions emerge from the interior of the Sun. It is believed that the solar dynamo at the shear layer at the bottom of the convection zone generates flux ropes, which emerge to the photosphere as active regions. The active regions emerge with stressed and concentrated magnetic field up to a few thousand Gauss. Following the emerging phase, the field evolves and decays. The decay process of active regions is not fully understood. Active regions usually have multiple flares and CMEs. Solar eruptions consume magnetic free energy in active regions and eject field and mass away from the Sun. Solar eruptions may play a role in the decay of the magnetic field in active regions. The lifetime of active regions range from hours to perhaps a few months. Stronger active regions usually live longer than the earth view pass. We had always a single view of the Sun before STEREO. Using the full sun imaging of the STEREO mission, we study a few recent active regions on the rise phase of solar cycle 24. When the regions are in earth view, we analyze HMI magnetograms for the field and energy evolution. By observing the total number of flares and CMEs from each region using STEREO coronal images, we estimate the released energy through the lifetime of these active regions. We discuss the implications to active region energy budget and active region decay.
Fisher George H.
Li Yadong
Luhmann Janet G.
Lynch Benjamin J.
Welsch Brian Thomas
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