HR: 09:15h
AN: SP31A-04    [Abstracts]
TI: Unified Mechanism for the Formation of Moving Magnetic Features
AU: * Ryutova, M P
EM: ryutova1@llnl.gov
AF: Lawrence Livermore National Laboratory/IGPP, 7000 East Ave, Livermore, CA 94550 United States
AU: Hagenaar, H J
EM: hagenaar@lmsal.com
AF: Lockheed Martin Advanced Technology Center, 3251 Hanover Street, Palo Alto, CA 94304 United States
AB: In the highly dynamic environment around sunspots there are small scale magnetic features, MMF's, that show clear regularities and may be thus categorized according their observed properties. For now there are at least 4 types of "MMF's" (Moving Magnetic Features). Type I MMF's are compact pairs of opposite polarity elements that may emerge anywhere in penumbra or moat region and move radially outward gradually separating; their velocities exceed the velocities of ambient flows, and their inner " foot" shares the sunspot's polarity. Type II MMF's are seen as unipolar features of the same polarity as the sunspot, moving outward from the sunspot with higher velocities than type I. Type III MMF's are also seen as unipolar features but have the polarity opposite to the sunspot's and travel with higher velocities than the other two types of MMF's. Recently the "type IV" features were observed in a sunspot formation region, that appear as compact bipoles flowing into sunspots and with an inner foot of a polarity opposite to the sunspot's. These were dubbed the MDF's (Moving Dipolar Features). The observed properties of all types of MMF's clearly violate the energy and momentum conservation laws, and thus require the application of physical mechanisms adequate for energetically open systems. Such mechanisms have been applied to type I and type II MMF's (Ryutova, Shine, Title, and Sakai, 1998, ApJ, 492, 402) with a good agreement between the theory and observations. Here we show that the same approach not only explains the origin, structure and dynamics of MDF's and type III MMF's, but consolidates all types of MMF's into one scheme. Theoretical results are compared with the observed properties of MMF's using time series of several data sets.
DE: 7524 Magnetic fields
DE: 7529 Photosphere
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly