Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.4108d&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #41.08; Bulletin of the American Astronomical Society, Vol. 24, p.795
Astronomy and Astrophysics
Astronomy
Scientific paper
We present observations by several instruments of the white-light flare (WLF) of 1991 June 9 01:34 UT. A white-light image from the National Astronomical Observatory of Japan indicates the location of the WLF within the active region (NOAA 6659). Stokes polarimetry from Mees Solar Observatory (University of Hawai`i) yields a vector magnetogram and a map of the vertical electric currents. Also from Mees comes Hα imaging spectroscopy, which is an indicator of such specific chromospheric processes as nonthermal electron precipitation, high coronal pressure, and mass motion. Both Mees instruments provide continuum images, allowing coregistration of the various datasets. The white-light emission arises from an extended area including both sunspot umbra and penumbra. The active region magnetic field is strongly nonpotential and has numerous vertical electric current channels. The WLF is situated in an area of relatively low current density at the edge of the strongest current in the active region, and the nearby magnetic neutral line is highly sheared. The WLF site shows electron precipitation, but only in its penumbral portion; stronger magnetic mirroring in the umbra may inhibit precipitation there. Also, the precipitation is not especially strong (relative to that observed elsewhere in this flare), suggesting that the electron-beam model for WLFs is not appropriate in this case. Also, the lack of strong redshifts argues against a dynamical energy transport model.
Canfield Richard C.
de La Beaujardiere Jean-Francois
Hiei Eijiro
Ichimoto Kiyoshi
Metcalf Thomas R.
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