Other
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1612h&link_type=abstract
American Astronomical Society, SPD meeting #42, #16.12; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
In early August 2010, HMI observed two long solar filaments of the new solar cycle that each erupted, yielding large CMEs, within a day of each other. One explanation for the cause of a CME is that the magnetic field of a filament becomes unstable due to twisting of the field by the turbulent convective flows near its footpoints. A CME results when the relatively cool filament gas supported by the field is expelled, along with significant amounts of energy, due to a reconnection event caused by the magnetic instability. It is thus of interest, for theories of coronal mass ejections from otherwise quiescent filaments, to know what the horizontal subsurface flows near the footpoints of the magnetic field are doing. In the work presented here, we extend our earlier ring-diagram analysis of subsurface flows near the neutral lines of these two filaments to include information from greater depths. This is due, in part, to our ability to measure flows from solar 5-minute oscillations of greater radial order and lower wavenumber through the use of multiple-ridge fitting of the power spectra than with the standard ring analysis technique. It is also due to our further use of our relatively new 3-D inversion code. This code combines information from 2, 4, and 16 degree tiles to determine self-consistent flows; preserving the high spatial resolution information provided by the small tiles with the greater depth information provided by the large tiles. The data used in this analysis were obtained with the HMI and AIA instruments on SDO as well as the H-alpha network. This work is supported by grants from NASA and institutional funding from NSF.
Bogart Richard. S.
Featherstone Nicholas
Haber Deborah A.
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