Mass loss on the main sequence

Details Mass loss on the main sequence Mass loss on the main sequence

Apr 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987comap..12...17w&link_type=abstract

Comments on Modern Physics, Part C - Comments on Astrophysics (ISSN 0146-2970), vol. 12, April 1987, p. 17-34.

Astronomy and Astrophysics

Astrophysics

69

Main Sequence Stars, Mass Flow Rate, Stellar Evolution, Stellar Mass Ejection, A Stars, Blue Stars, Chemical Evolution, G Stars, Galactic Evolution, Globular Clusters, Gravitational Collapse

Scientific paper

The hypothesis is advanced that stars on the main sequence in the pulsation-instability strip lose mass at rates in excess of 10 to the -9th solar mass/yr and thus evolve down the main sequence. The mass-loss rate is expected to diminish steeply when the convective surface layers become substantial. As a result, a significant fraction of early G stars in populations more than 1 Gyr old were A stars when they commenced core hydrogen burning. Among other consequences, such mass loss will cause some clusters to appear much older than they are, suggesting a resolution to the apparent conflict between current estimates for the ages of globular clusters and other recent determinations of the age of the Galaxy and the universe. This hypothesis leads to an explanation for blue stragglers, has implications for the chemical evolution of the Galaxy, and alters the mass function of stars on the main sequence. It is also suggested that the sun was such a star, arriving on the main sequence with M = 2 solar masses and losing the excess over about 1 Gyr.

Affiliated with

Also associated with

No associations

Rating

Mass loss on the main sequence does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Mass loss on the main sequence, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Mass loss on the main sequence will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1347822