Quantitative Constraints for Massive Star Evolution Models with Rotation

Details Quantitative Constraints for Massive Star Evolution Models with Rotation Quantitative Constraints for Massive Star Evolution Models with Rotation

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9437v&link_type=abstract

HST Proposal ID #9437

Physics

Hst Proposal Id #9437

Scientific paper

Rotation is now recognized as an important physical component in understanding massive stars. Theory suggests that rotation affects the lifetimes, chemical yields, stellar evolution tracks, and the supernova and compact remnant properties {Heger & Langer 2000, Maeder & Meynet 2000}. In a Cycle 7 program, we proved that rotational mixing occurs in massive main sequence stars {Venn et al. 2001}. In this proposal, we want to quantitatively test model predictions and constrain the theory for a better understanding of massive star evolution. We are requesting HST STIS observations of the BIII 2066 Angstrom resonance line of seven massive stars in three young clusters carefully selected from IUE analyses. These stars show traces of boron depletion, but without nitrogen enrichment; rotation is the only theory able to explain this abundance pattern. These new abundances will allow us to test rotating model predictions: that mixing strength increases with stellar age, mass, and rotation rate. They will also help to quantitatively constrain the rotational mixing efficiencies in massive stars. One very high S/N spectrum of a moderately boron-depleted star is also requested. We wish to measure its 11B/10B ratio, which is predicted to change as boron is depleted in the rotating models. This ratio will further confirm rotational effects and observationally constrain the 10B{p, Alpha} thermonuclear reaction rate, which is presently highly uncertain.

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