| Issue |
A&A
Volume 387, Number 2, May IV 2002
|
|
|---|---|---|
| Page(s) | 595 - 604 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20020421 | |
| Published online | 13 May 2002 | |
Some aspects of the calculation of Balmer lines in the sun and stars*
1
Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1090 USA
2
Istituto di Astrofisica Spaziale e Fisica Cosmica, CNR, via del Fosso del Cavaliere, 00133 Roma, Italy
3
Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy, e-mail: castelli@ts.astro.it
Corresponding author: C. Cowley, cowley@astro.lsa.umich.edu
Received:
9
January
2002
Accepted:
18
March
2002
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 Hα through Hδ 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.
Key words: stars: atmospheres / stars: fundamental parameters / line: formation / line: profiles
© ESO, 2002
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