Modelling Active Region Magnetic Fields in the Context of the Global Corona

Details Modelling Active Region Magnetic Fields in the Context of the Global Corona Modelling Active Region Magnetic Fields in the Context of the Global Corona

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..61l&link_type=abstract

Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R

Physics

Scientific paper

Coronal mass ejections (CMEs) disrupt the large-scale coronal magnetic field and propel plasma and magnetic flux outward into interplanetary space. The fastest and most energetic CMEs typically originate from active regions on the Sun. For active region CMEs both the local active region magnetic field and the global magnetic fields due to the surrounding magnetic flux are important. Modelling active region magnetic fields in the context of the global corona presents special challenges, due to the range of scales involved and the strong magnetic fields present in active regions. This regime requires more accurate coronal models that include energy transport (radiative losses, anisotropic thermal conduction, and coronal heating) in the transition region. In this talk we describe MHD models of active region fields embedded in the global corona, and we discuss their eruptive properties. We discuss the implications of our work for the initiation of fast CMEs. Work supported by NASA, NSF and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).

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