Is the Mn I 539.4 nm Variation with Activity Explained?

Details Is the Mn I 539.4 nm Variation with Activity Explained? Is the Mn I 539.4 nm Variation with Activity Explained?

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..368..543v&link_type=abstract

The Physics of Chromospheric Plasmas ASP Conference Series, Vol. 368, Proceedings of the conference held 9-13 October, 2006 at t

Physics

1

Scientific paper

The photospheric Mn I 539.4 nm line in the solar spectrum shows unusual variability with the solar cycle in that its depth decreases with increasing activity. \citet{nv-2001A&A...369L..13D} claimed that this phenomenon is due to interlocking between the chromospheric Mg II h & k lines and an overlapping Mn I multiplet. In this contribution we test this hypothesis by synthesizing Mn I 539.4 nm line including these interlocking lines for a range of standard solar models and then combining resulting profiles without and with interlocking to emulate the full-disk profile variation. We find that the interlocking gives only a minor contribution; the largest one comes from different temperature stratifications in the photospheric layers of the various models.

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