Other
Scientific paper
Apr 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aps..aprq20010n&link_type=abstract
American Physical Society, April Meeting, April 29-May 2, 2000 Long Beach, CA, abstract #Q20.010
Other
Scientific paper
Thermal emission from a rotating, supermassive star will cause the configuration to contract slowly and spin up. If internal viscosity and magnetic fields are sufficiently weak, the contracting star will rotate differentially. In this limit, the fate of a cooling supermassive star depends sensitively on its initial angular momentum distribution. If the star is nearly spherical and in uniform rotation initially, then cooling and contraction will cause it to flatten and spin up to the mass-shedding limit. Subsequent cooling may lead to mass and angular momentum loss which might eventually drive the configuration to the onset of dynamical collapse. However, for other initial profiles characterized by differential rotation, mass-shedding limits do not always exist along an evolutionary sequence. Instead, a supermassive star will encounter the dynamical bar-mode instability, which may trigger the growth of nonaxisymmetric bars. Either scenario may lead to the generation of long wavelength gravitational waves, which could be detectable by future space-based laser interferometers like LISA.
New Kimberly
Shapiro Stuart
No associations
LandOfFree
Evolution of Rotating Supermassive Stars: Low-Viscosity Limit 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 Rotating Supermassive Stars: Low-Viscosity Limit, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Evolution of Rotating Supermassive Stars: Low-Viscosity Limit will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-752208