Inferring plasma flow velocities from photospheric vector magnetic field observations for the investigation of flare onsets

Details Inferring plasma flow velocities from photospheric vector magnetic field observations for the investigation of flare onsets Inferring plasma flow velocities from photospheric vector magnetic field observations for the investigation of flare onsets

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008adspr..42..812s&link_type=abstract

Advances in Space Research, Volume 42, Issue 5, p. 812-821.

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The amount of emergence and submergence of magnetized plasma and the horizontal motion of the footpoints of flux tubes might be crucial for the dynamics of the solar atmosphere. Although the rate of flux emergence and submergence can be observationally determined near the polarity inversion line (Chae et al., 2004), the same is not true for regions away from the PIL. Also, the horizontal motions cannot be directly measured in the solar photosphere. In this sense, the evolution of the photospheric magnetic field provides valuable information which can be used to estimate photospheric plasma flows since magnetic field and plasma are closely associated (frozen-in-condition). We used three methods to estimate the photospheric plasma motion from magnetic field observations. The methods were applied to photospheric vector magnetic field data of active region NOAA 9077, observed by the Huairou Solar Observing Station (HSOS) of the National Astronomical Observatories of China before and after the ‘Bastille Day’ flare on July 13th and 14th, 2000.

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