HR: 1340h
AN: SH53A-1073    [Abstracts]
TI: Photospheric Magnetic Flux Emergence: A comparative study between Hinode/SOT Observations and MHD simulations
AU: * Cheung, M C
EM: cheung@lmsal.com
AF: Lockheed Martin Solar and Astrophysics Laboratory, Bldg. / 252 Org./ L9-41 3251 Hanover Street, Palo Alto, CA 94304, United States
AU: Schüssler, M
EM: msch@mps.mpg.de
AF: Max Planck Institute for Solar System Research, Max-Planck-Str. 2, Katlenburg-Lindau, 37191, Germany
AU: Moreno-Insertis, F
EM: fmi@iac.es
AF: Instituto de Astrofísica de Canarias, C/ Vía Láctea, s/n, La Laguna, E38205, Spain
AU: Tarbell, T D
EM: tarbell@lmsal.com
AF: Lockheed Martin Solar and Astrophysics Laboratory, Bldg. / 252 Org./ L9-41 3251 Hanover Street, Palo Alto, CA 94304, United States
AB: With high angular resolution, high temporal cadence and a stable point spread function, the Solar Optical Telescope (SOT) onboard the Hinode satellite is the ideal instrument for the study of magnetic flux emergence and its manifestations on the solar surface. In this presentation, we focus on the development of ephemeral regions and small active regions. In many instances, SOT has been able to capture the entire emergence process from beginning to end: i.e. from the initial stages of flux appearance in granule interiors, through the intermediate stages of G-band bright point formation, and finally to the coalescence of small vertical flux elements to form pores. To investigate the physics of the flux emergence process, we performed 3D numerical MHD simulations with the MURaM code. The models are able to reproduce, and help us explain, various observational signatures of magnetic flux emergence.
DE: 7524 Magnetic fields
DE: 7529 Photosphere
DE: 7599 General or miscellaneous
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting