Line Profile Variations in Be-Stars

Details Line Profile Variations in Be-Stars Line Profile Variations in Be-Stars

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.153...61a&link_type=abstract

Astrophysics and Space Science, Volume 153, Issue 1, pp.61-66

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Be stars show both emission and absorption profiles in the optical part of the spectrum, and these are found to vary with the time. Some of the shifts in profiles were earlier interpreted as Doppler shifts. However, some of the shifts of features in both emission and absorption line profiles may be artifacts due to superposition of an emission profile arising from an H ii region around a binary compact object, and a profile due to the Be star. This interpretation of shifts in line profiles has the advantage over the conventional Doppler-shift interpretation in so far as it does not need the oscillation of a large mass of circumstellar gas, and leads to the observed correlation between radial velocity (RV) variations and V/R variations.

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