Formation of Moving Magnetic Features and Penumbral Magnetic Fields

Details Formation of Moving Magnetic Features and Penumbral Magnetic Fields Formation of Moving Magnetic Features and Penumbral Magnetic Fields

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9410k&link_type=abstract

American Astronomical Society Meeting 210, #94.10; Bulletin of the American Astronomical Society, Vol. 39, p.218

Astronomy and Astrophysics

Astronomy

Scientific paper

We investigate the formation process of Moving Magnetic Features (MMFs) observed with Hinode/SOT. Moving magnetic features are small magnetic elements moving outward in the moat region surrounding mature sunspots. We derive vector magnetic fields of MMFs around simple sunspots near the disk center. Most of MMFs with polarity opposite to the sunspot have large redshift around the penumbral outer boundary. We find that some of them have Doppler velocities of about 10 km/s and such large Doppler motion is observed only in the Stokes V profile. The Stokes Q and U profiles in the same pixel do not have any significant Doppler motions. Horizontal magnetic fields of the penumbra frequently extend to the moat region and the MMFs having horizontal fields with polarity same as the sunspot are formed. The MMFs with polarity opposite to the sunspot appear around the outer edge of the extending penumbral fields. We also find penumbral spines, which have more vertical magnetic fields than the surroundings, branch off at their outer edge and MMFs having relatively vertical fields with polarity same as the sunspot are detached from the outer edge of the branch. The branch of penumbral spine is formed when granular cells in the moat region go into the penumbra.

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