Binary Mass Transfer and the Spin-Up of Massive Stars

Details Binary Mass Transfer and the Spin-Up of Massive Stars Binary Mass Transfer and the Spin-Up of Massive Stars

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..234g&link_type=abstract

NOAO Proposal ID #2000B-0234

Computer Science

Scientific paper

The origin and cause of the rapidly rotating Be stars is still a mystery after a century of study. A promising explanation is that these stars were spun-up through mass transfer in close binaries, and in most cases the companions are now too faint to detect. This theory predicts that the projected rotational velocity distribution of massive stars should develop a high velocity component after enough time has elapsed for the first stars to begin Roche lobe overflow (approximately 10 Myr for early B-type stars). Here we propose to obtain spectroscopy of massive stars in 14 populous clusters younger than 25 Myr in order to search for the emergence of rapid rotators in the older group. The spectra will also be used to: (1) search for an early spin-down in massive stars in order to estimate what magnetic fields are present, (2) search for a proposed He enrichment with age due to mixing, (3) estimate the incidence of spectroscopic binaries in clusters of different ages, and (4) study the radial velocities and dynamics of the massive star population. A companion study of 14 southern clusters is scheduled for April, 2000, with the CTIO 4-m and Hydra spectrograph.

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