Some Aspects of the calculation of Balmer lines in the sun and stars

Abstract

We compare the results of Balmer-line calculations using recent theory and improved computational algorithms with those from the widely-used SYNTHE and BALMER9 routines. The resulting profiles are mostly indistinguishable. Good fits to the normalized solar Balmer lines H$\hat{I}\pm$ through H$\hat{I}´$ are obtained (apart from the cores) using the recent unified-broadening calculations by Barklem and his coworkers provided that some adjustment for the continuum is performed. We discuss a surprising linearity with temperature of the Balmer line profiles in dwarfs.

Submitted to Astronomy and Astrophysics Better figures at http://astro.lsa.umich.edu/users/cowley