The problem of runaway stars and the distribution function of peculiar radial velocities in the Large Magellanic Cloud

Details The problem of runaway stars and the distribution function of peculiar radial velocities in the Large Magellanic Cloud The problem of runaway stars and the distribution function of peculiar radial velocities in the Large Magellanic Cloud

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...152..343i&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 152, no. 2, Nov. 1985, p. 343-348. In German.

Astronomy and Astrophysics

Astrophysics

Binary Stars, Distribution Functions, Interstellar Gas, Magellanic Clouds, Radial Velocity, Stellar Evolution, Stellar Mass Accretion, Supergiant Stars, Supernovae

Scientific paper

Distribution functions of peculiar radial velocities in the Large Magellanic Cloud (LMC) are studied. The velocity dispersion obtained after correcting for observing errors is 7 km/s for the interstellar hydrogen and 14 km/s for the supergiants. This suggests that the process of (secondary?) star formation in the LMC leads to an increase of the velocity dispersion of approximately 12 km/s. The distribution function of the peculiar radial velocities of supergiants is purely Gaussian. There is no significant evidence for runaway stars in the LMC. The consequences of this finding with regard to the three current hypotheses for the formation of runaway stars are discussed. It is shown that the runaways certainly do not escape from protoclusters nor do they belong to the old disk population as 'subluminous O-stars'. Only the origin in close binary systems after mass transfer and supernova explosion of the primary appears to be a viable solution to the runaway star problem, but in this case the orientation of the orbital planes of massive close binary systems should be strongly concentrated to that of the galactic plane.

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