Rapid changes of sunspot structure associated with solar eruptions

Details Rapid changes of sunspot structure associated with solar eruptions Rapid changes of sunspot structure associated with solar eruptions

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..273...15w&link_type=abstract

The Physics of Sun and Star Spots, Proceedings of the International Astronomical Union, IAU Symposium, Volume 273, p. 15-20

Physics

Sun: Activity, Sun: Flares, Sun: Coronal Mass Ejections (Cmes), Sun: Magnetic Fields

Scientific paper

In this paper we summarize the studies of flare-related changes of photospheric magnetic fields. When vector magnetograms are available, we always find an increase of transverse field at the polarity inversion line (PIL). We also discuss 1 minute cadence line-of-sight MDI magnetogram observations, which usually show prominent changes of magnetic flux contained in the flaring δ spot region. The observed limb-ward flux increases while disk-ward flux decreases rapidly and irreversibly after flares. These observations provides evidences, either direct or indirect, for the theory and prediction of Hudson, Fisher & Welsch (2008) that the photospheric magnetic fields would respond to coronal field restructuring and turn to a more horizontal state near the PIL after eruptions. From the white-light observations, we find that at flaring PIL, the structure becomes darker after an eruption, while the peripheral penumbrae decay. Using high-resolution Hinode data, we find evidence that only dark fibrils in the ``uncombed'' penumbral structure disappear while the bright grains evolve to G-band bright points after flares.

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