The formation of Be stars in close binary systems. The importance of kicks and angular-momentum loss

Details The formation of Be stars in close binary systems. The importance of kicks and angular-momentum loss The formation of Be stars in close binary systems. The importance of kicks and angular-momentum loss

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...296..691p&link_type=abstract

Astronomy and Astrophysics, v.296, p.691

Astronomy and Astrophysics

Astrophysics

34

Stars: Binaries: Close, Stars: Be, Stars: Supernovae, Stars: Evolution

Scientific paper

With a simplified model for case B close binary-evolution, the production of Be stars and companions is studied in order to address the observation that all Be stars with a neutron-star companion (~30) are more massive than about 8Msun_ (spectral type earlier than B2.5). In the model we assume that Be stars are formed in binary systems where mass transfer spins up the accretor to high rotational velocity so that it starts showing the Be-effect. Since mass transfer is thought to occur on a relatively short timescale, the Be stars will be accompanied by a helium star (mass-transfer remnant), a white dwarf or a neutron star. Kicks (of the order of 100 to 200km/s), as result of a non-symmetric supernova event, reduce the number of late type Be stars with a neutron-star companion only slightly and thus do not seem to satisfy the observational constraint. If during non-conservative binary-evolution, mass lost from the system is removed with the specific angular-momentum per unit mass at the second Lagrange point, systems with small initial mass ratios do not evolve into Be x-ray binaries. Consequently, no Be stars with a neutron-star companion are formed with a spectral type later than B2.5, in good agreement with the observations.

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