Why solar magnetic flux concentrations are bright in molecular bands

Schüssler, M., Shelyag, S., Berdyugina, S., Vögler, A. and Solanki, S. K. 2003, Why solar magnetic flux concentrations are bright in molecular bands, The astrophysical journal letters, vol. 597, no. 2, pp. 173-176, doi: 10.1086/379869.

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Title Why solar magnetic flux concentrations are bright in molecular bands
Author(s) Schüssler, M.
Shelyag, S.ORCID iD for Shelyag, S. orcid.org/0000-0002-6436-9347
Berdyugina, S.
Vögler, A.
Solanki, S. K.
Journal name The astrophysical journal letters
Volume number 597
Issue number 2
Start page 173
End page 176
Total pages 4
Publisher IOP Publishing
Place of publication Bristol, Eng.
Publication date 2003-10-17
ISSN 0004-637X
Summary 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.
Language eng
DOI 10.1086/379869
Field of Research 0201 Astronomical And Space Sciences
0305 Organic Chemistry
0306 Physical Chemistry (Incl. Structural)
HERDC Research category CN.1 Other journal article
Copyright notice ©2003, The American Astronomical Society
Persistent URL http://hdl.handle.net/10536/DRO/DU:30114981

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