Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...5e...9y&link_type=abstract
Calibrating the Top of the Stellar M-L Relation, 26th meeting of the IAU, Joint Discussion 5, 16 August 2006, Prague, Czech Repu
Computer Science
Scientific paper
One of the common scenarios for the formation of Ultraluminous X-Ray Sources implies the formation of an accreting black hole from an ultramassive object created by a hierarchical runaway merger of stars in a young dense stellar cluster during or after core collapse. Very massive stars are found in young Galactic clusters. We find that the upper limit of masses of nonrotating homogeneous solar metallicity stars is close to 1000 solar masses. We compute the evolution of M=(100 - 1000) solar mass stars from the ZAMS to core-helium exhaustion. We apply a mass-loss algorithm that takes into account the relation between stellar luminosity and Eddington luminosity. At the lower limit of the mass-range under consideration, our results are consistent with observations in reproducing the Humphreys-Davidson limit. We can reproduce the position of the bulk of the most massive Galactic and MC stars in the HR-diagram and the mass-loss rates observed for stars in the Arches and Quintuplet clusters We show that the evolution of ultra-massive solar metallicity stars results either in pair-creation supernovae leaving no remnant or in the formation of black holes with mass lower than about 60 solar masses.
No associations
LandOfFree
Evolution of Ultra-Massive Stars and its Implications 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 Evolution of Ultra-Massive Stars and its Implications, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Evolution of Ultra-Massive Stars and its Implications will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1783561