Computer Science
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982iaus...98..311p&link_type=abstract
In: Be stars; Proceedings of the Symposium, Munich, West Germany, April 6-10, 1981. (A83-10301 01-90) Dordrecht, D. Reidel Publi
Computer Science
3
B Stars, Binary Stars, Radial Velocity, Stellar Motions, Stellar Spectra, Line Spectra, Mass Transfer, Stellar Envelopes, Stellar Evolution, Stellar Models
Scientific paper
It is suggested that the primary reason for the reluctance of researchers to accept the binary hypothesis concerning Be star behavior is that few such stars have been confirmed to be spectroscopic binaries. Obstacles to the detection of binary motion include the expectation that the semiamplitude for the radial velocity will be small, while spectral lines are often broad, complex features containing both absorption and weak emission components that render measurements more uncertain than those for sharp symmetrical lines. The recent determination of orbits for two relatively long period interacting binary Be stars, HR 2142 and Phi Per, are discussed in light of the semiamplitude value problem.
No associations
LandOfFree
Be stars as interacting binaries does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Be stars as interacting binaries, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Be stars as interacting binaries will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-842022