Why Solar Magnetic Flux Concentrations Are Bright in Molecular Bands

Details Why Solar Magnetic Flux Concentrations Are Bright in Molecular Bands Why Solar Magnetic Flux Concentrations Are Bright in Molecular Bands

Nov 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...597l.173s&link_type=abstract

The Astrophysical Journal, Volume 597, Issue 2, pp. L173-L176.

Astronomy and Astrophysics

Astronomy

51

Sun: Magnetic Fields, Sun: Photosphere

Scientific paper

Using realistic ab initio simulations of radiative magnetoconvection, we show that the bright structures in images taken in the ``G band,'' a spectral band dominated by lines of the CH molecule, precisely outline small-scale concentrations of strong magnetic fields on the visible solar surface. The brightening is caused by a depletion of CH molecules in the hot and tenuous magnetic structures, thus confirming the model of radiatively heated magnetic flux concentrations. These results provide a firm basis for observational studies of the evolution and dynamics of the small-scale solar magnetic field derived through ``proxy magnetometry'' with G-band images.

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