Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars

Details Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6571p&link_type=abstract

HST Proposal ID #6571

Physics

Hst Proposal Id #6571 Hot Stars

Scientific paper

The key to understanding main sequence evolution is hidden inthe detailed knowledge of the interiors of white dwarfs, theendpoints of stellar evolution. Unfortunately, we do notunderstand these objects. We find structural differencesamong the two major groups of white dwarfs (hydrogen vs heliumphotospheres) that demand differences in origin which are notclearly understood by our current models. In 1992, HSTobtained high quality, high resolution spectra of the wellstudied helium (DB) white dwarf PG1645+325 (GD358), amultiperiodic g-mode pulsator, detecting CII (1335 Angstrom)and HeII (1640Angstrom). Our results imply a thin heliumlayer mass, in agreement with the asteroseismology (10^-6rmMSUN) and in disagreement with the conventional wisdom ofstellar evolution. We propose using carbon to probe theenvelope structure of the hotter DB white dwarfs.

Affiliated with

Also associated with

No associations

Rating

Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars 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 Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Carbon and Convective Mixing in Hot Helium Rich White Dwarf Stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1117907