A study of Balmer decrements in Be star emission-line spectra

Details A study of Balmer decrements in Be star emission-line spectra A study of Balmer decrements in Be star emission-line spectra

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...238..227d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 238, no. 1-2, Nov. 1990, p. 227-241.

Astronomy and Astrophysics

Astrophysics

13

B Stars, Balmer Series, Emission Spectra, Stellar Spectra, Error Analysis, H Lines, Spectral Line Width, Stellar Envelopes

Scientific paper

Balmer decrements are determined for 26 bright equatorial and southern early-Be type stars and are compared with theoretical Balmer decrements calculated for high-density hydrogen nebulae resembling typical conditions expected for circumstellar envelopes around Be stars. The derived Balmer decrement values comprise rather narrow ranges, at most D(34) between 1.2 and 3.2 and D(54) between 0.4 and 1.0. Weak emission-line Be stars are often characterized by relatively flat Balmer decrements. Among Be stars, very steep Balmer decrements are only observed for Be shell stars. The main parameter governing the value of Balmer decrements appears to be the mean electron density in the circumstellar envelope.

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