The velocity-mass correlation of the O-type stars - Model results

Details The velocity-mass correlation of the O-type stars - Model results The velocity-mass correlation of the O-type stars - Model results

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982aj.....87...90s&link_type=abstract

Astronomical Journal, vol. 87, Jan. 1982, p. 90-97.

Astronomy and Astrophysics

Astronomy

33

Binary Stars, Mass Flow Rate, O Stars, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Drift Rate, Helium, Main Sequence Stars, Mass Ratios, Roche Limit, Stellar Winds, Supernovae

Scientific paper

New results are presented for a model describing massive close binary evolution from initial ZAMS to post-supernova stages, which explicitly allows for primary system mass loss during both primary star hydrogen- and helium-burning stages and Roche lobe overflow. The model results consistently predict (1) an increasing relation between runaway OB star peculiar space velocities and masses, which is in agreement with observed correlations, and (2) an 11-solar mass lower limit for the masses of runaway stars, in agreement with the observational limit found by Blaauw (1961). It is also predicted that the more massive O stars will produce correspondingly more massive compact remnants and that most binaries experiencing supernova-induced kick velocities greater than about 300 km/sec will disrupt following the explosions. In light of pulsar-observation estimates of this velocity of about 150 km/sec, only 15% of these binaries are likely to be disrupted by the supernova explosions and all runaway stars should have either neutron star or black hole companions.

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