The Degenerate Remnant Cores of Ultra--Metal--Poor Heavy--Weight Intermediate Mass Stars: White Dwarfs or Supernovae?

Details The Degenerate Remnant Cores of Ultra--Metal--Poor Heavy--Weight Intermediate Mass Stars: White Dwarfs or Supernovae? The Degenerate Remnant Cores of Ultra--Metal--Poor Heavy--Weight Intermediate Mass Stars: White Dwarfs or Supernovae?

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..372....9g&link_type=abstract

15th European Workshop on White Dwarfs ASP Conference Series, Vol. 372, proceedings of the conference held 7-11 August, 2006 in

Astronomy and Astrophysics

Astronomy

Scientific paper

We have computed the evolution of heavy--weight intermediate mass primordial stars with masses at the main sequence ranging from 5 to 10 Msun. Our calculations encompass from the main sequence until the early stages of the TP-(S)AGB phase and have been performed both disregarding overshooting and considering a moderate amount of it. We have found that the evolution and the final remnants of a star computed with overshooting is similar to that of a star of a mass ˜ 2 Msun larger computed without overshooting. We have also determined the minimum ZAMS mass required to develop extensive carbon burning and, therefore, resulting in ONe cores after the main nuclear evolutionary stages. This minimum mass is about 7.5 Msun for the case in which overshooting was disregarded and 6 Msun for the case in which it was taken into account. Finally, we discuss the different possibilities for the final fate of these stars. We also comment on the uncertainties associated to the lack of reliable mass loss prescriptions for ultra--metal--poor stars set on our knowledge of the final fate of primordial stars.

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