The formation and detectability of Be + white dwarf systems

Details The formation and detectability of Be + white dwarf systems The formation and detectability of Be + white dwarf systems

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...220l...1w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 220, no. 1-2, Aug. 1989, p. L1-L4.

Astronomy and Astrophysics

Astrophysics

37

B Stars, Binary Stars, Stellar Evolution, Stellar Systems, White Dwarf Stars, X Ray Binaries, Mass Transfer, Stellar Luminosity, Stellar Mass Accretion

Scientific paper

The formation of Be + He star and Be + white dwarf binaries is discussed using evolutionary calculations. A total number of 300-1000 rapidly rotating B star + He star binaries and 100-300 rapidly B star + white dwarf binaries should exist within 1 kpc of the sun. If the B star is a Be star, the Be + white dwarf systems produce X-rays due to accretion of wind material of the equatorial wind of the Be star onto the white dwarf. The estimated X-ray luminosities range between 10 to the 29th and 10 to the 33rd erg/s. The late type Be stars Mu2 Cru and HR 4804, that have X-ray luminosities of about 10 to the 32nd erg/s, are likely to have accreting white dwarf companions. The Be stars with unseen companions are good candidates for Be + He star binaries.

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