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Astronomy & Astrophysics manuscript no. (will be inserted by hand later)

Summary: Astronomy & Astrophysics manuscript no.
(will be inserted by hand later)
Solar Mn I 5432/5395š A line formation explained
J.G. Doyle 1 , D. Jevremovi'c 1;2 , C.I. Short 3 , P.H. Hauschildt 4 , W. Livingston 5
, and I. Vince 2
1 Armagh Observatory, College Hill, Armagh BT61 9DG, N. Ireland
2 Astronomical Observatory, Volgina 7, 11050 Belgrade, Yugoslavia
3 Dept of Phys, Charles E. Schmidt College of Science, Florida Atlantic University, Boca Raton, FL, 33431, USA
4 Dept of Phys & Astron and Center for Simulational Physics, University of Georgia, Athens, GA, 30602, USA
5 National Solar Observatory, NOAO ? , P.O. Box 26732, Tucson, AZ 85726, USA
emails: jgd@star.arm.ac.uk, djc@star.arm.ac.uk, ishort@acc.fau.edu, yeti@hal.physast.uga.edu, wcl@noao.edu,
Received date, accepted date
Abstract. We present a solution for the long standing problem concerning the `chromospheric' behaviour of the
Mn i 5395/5432 š A lines in the solar spectrum using multi­line/multi­species NLTE modelling. Using comprehensive
spectral line formation modelling, we show that the Mn i lines are very sensitive to optical pumping in a transition
which overlaps with Mg ii k. It therefore follows that one has to be careful with the choice of lines as temperature
indicators and for the determination of the Mn abundances although on the other hand, due to the formation
process of these lines they may be useful as a solar and stellar activity diagnostic.
Key words. Mn i line formation --- solar chromosphere --- NLTE modelling --- radiative interaction


Source: Armagh Observatory


Collections: Physics