New possible binaries among B(e) stars

Details New possible binaries among B(e) stars New possible binaries among B(e) stars

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26at....6..251m&link_type=abstract

Astronomical and Astrophysical Transactions (ISSN 1055-6796), vol. 6, no. 4, p. 251-263

Astronomy and Astrophysics

Astrophysics

20

B Stars, Binary Stars, Emission Spectra, Main Sequence Stars, Shell Stars, Stellar Envelopes, Astronomical Photometry, Astronomical Spectroscopy, Balmer Series, Cosmic Dust, Interstellar Gas, Spectral Energy Distribution

Scientific paper

The majority of B(e) stars are probably Post-Main-Sequence objects with circumstellar dust shells. Their complicated spectral energy distributions (SED) and line spectra make the determination of the object composition very difficult. We present here the results of new photometric and spectral observations of the B(e) star MWC 84 and MWC 930, similar to B(e)-s, and show that they are possible binaries. It is shown that MWC 84 consist of two stars with spectral types approximately KO II and BO V, a strong gas envelope, and a dust shell with the optical depth about 0.1; MWC 930 probably consists of KO I and BO V stars, a gas envelope, and no circumstellar dust. An analysis of Balmer decrements for different emission-line objects is presented.

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