Studying Solar Active Regions with HMI Data

Details Studying Solar Active Regions with HMI Data Studying Solar Active Regions with HMI Data

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2102l&link_type=abstract

American Astronomical Society, SPD meeting #42, #21.02; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

Full disk field of view, continuous time coverage, high temporal and spatial resolutions, and consistent data quality, these specifications of the HMI observational data allows us to study in detail the evolution of solar active regions during the course from emerging to decaying. Using the HMI vector magnetic field data (test version), we study the magnetic energy and helicity in emerging active regions. First, we apply the code DAVE4VM (Schuck 2008) to the time-series vector magnetic field data to derive the plasma velocity; then we break down the energy and helicity fluxes into two components, one due to vertical advection of the magnetic field through the photosphere, and the other due to the horizontal motion that shears the field lines. We analyze the roles these two processes play in accumulating the energy and helicity in the corona, and explore their correlations with the evolution of active regions.

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