Physics
Scientific paper
Apr 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998eostr..79..282v&link_type=abstract
1998 Spring Meeting, American Geophysical Union, Supplement to EOS, April 28, 1998, abstract SH42D-8, p. S282
Physics
Convection, Solar Granulation, Solar Corona, Solar Magnetic Field
Scientific paper
The magnetic field in the solar photosphere interacts with convective flows on a variety of length and time scales. On the scale of the solar granulation the magnetic field is pushed into the intergranular lanes, producing magnetic flux concentrations with kilogauss field strength. In this talk I present results from a recent study (van Ballegooijen et al 1998) of the motions of these magnetic elements and their interaction with the granulation flow. The study is based on a time series of high resolution G-band (4305 Angstrom) and continuum (4686 Angstrom) images obtained at the Swedish Vacuum Solar Telescope at La Palma, Spain. The G-band images show bright points which are known to be associated with the magnetic flux concentrations. We use object tracking techniques to measure the motions of these bright points over a 70 minute period, and derive the autocorrelation function of the bright point velocity, which is found to vary on a time scale of about 100 s. We construct models of the granulation flow field and simulate the dynamics of magnetic elements assuming they are passively advected by these flows. Finally, we use potential field modeling to simulate magnetic and velocity fields above the observed region (up to a height of 1500 km in the chromosphere). The results indicate that the spreading of the magnetic flux tubes with height, and their merging in the chromosphere, produce local enhancements in velocity near the separatrix surfaces between the flux tubes in the chromosphere. The chromospheric velocity exceeds 5 km/s, much larger than the velocity of the underlying photospheric flux tubes. We suggest that such velocity enhancements play an important role in the generation of MHD waves and the formation of H-alpha spicules.
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