Solar Cycle Variation of the Ca 854.2 nm Line Bisectors

Details Solar Cycle Variation of the Ca 854.2 nm Line Bisectors Solar Cycle Variation of the Ca 854.2 nm Line Bisectors

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1703p&link_type=abstract

American Astronomical Society, SPD meeting #42, #17.03; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

The bisector of the strong chromospheric Ca II 854.2 nm line has an inverse-C shape the cause of which is not yet fully understood. We show that the amplitude of the bisector in Sun-as-a-star observations exhibits a solar cycle variation with smaller amplitudes during highest activity. The line core intensity is lower during solar minima while the part of the bisector most sensitive to the line core shows no systematic change with activity. We also show preliminary results of a connection between magnetic shadows and bisector amplitudes. Our results support the use of Ca II 854.2 nm bisectors in studying the relationship between convection and magnetic fields, not only in the Sun but in other stars as well.

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