High-resolution emission-line spectroscopy of Be stars. I - Evidence for a two-component structure of the H-alpha emitting envelope

Details High-resolution emission-line spectroscopy of Be stars. I - Evidence for a two-component structure of the H-alpha emitting envelope High-resolution emission-line spectroscopy of Be stars. I - Evidence for a two-component structure of the H-alpha emitting envelope

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...166..185h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 166, no. 1-2, Sept. 1986, p. 185-194.

Astronomy and Astrophysics

Astrophysics

46

B Stars, Emission Spectra, H Alpha Line, Stellar Spectra, Variable Stars, Flux Density, Radial Velocity, Rotating Disks, Signal To Noise Ratios, Southern Sky, Spectral Line Width

Scientific paper

An atlas of high-resolution (R = 50,000), high signal to noise ratio H-alpha profiles for 24 bright southern Be stars is presented. For a number of program stars, inflections in the flanks of the profiles are most easily explained by the assumption that the H-alpha profile is composed of two components, a relatively broad, strong primary and a narrow, weak secondary one. Double-peak structure of the secondary component is common for all v sin i values; the peak separation, being a characteristic of the second component, is correlated with the FWHM of the first component. A minimum value for FWHM of H-alpha is indicated by the H-alpha profile for the pole-on star HR 2825 (v sin i less than about 40 km/s) with FWHM = 115 km/s. For four program stars (Kappa CMa, HR 3237, Delta Cen, Chi Oph), the H-alpha profiles are highly asymmetric with either a strong, single peak or a strong peak combined with one or two weaker secondary peaks, indicating strong radial motions in the envelope.

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