Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...147..161e&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 147, no. 1, June 1985, p. 161-168.
Astronomy and Astrophysics
Astrophysics
28
Gravitational Collapse, Polytropic Processes, Stellar Cores, Stellar Rotation, Density Distribution, Stellar Evolution, Stellar Mass, Stellar Models
Scientific paper
Equilibrium models of axisymmetric, differentially rotating polytropes are used to estimate the properties of rotating stellar cores at the end point of their collapse. Results are presented for polytropes with adiabatic indices of 4.3, 1.32, 1.29, and 1.25. The results are in qualitative agreement with the results of earlier investigations, which did not allow for changes in the shape of the configuration, for the presence of density gradients, and for large differential rotation. The analysis shows that a rotating stellar core will not collapse all the way to neutron star densities on a dynamical time scale, if its initial ratio of rotational to gravitational energy is larger than some minimum value. The collapse stops due to rotation at an intermediate, dynamically stable, axisymmetric equilibrium state, and further evolution proceeds on a secular time scale.
Eriguchi Yoshiharu
Mueller Ewald
No associations
LandOfFree
Equilibrium models of differentially rotating polytropes and the collapse of rotating stellar cores 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 Equilibrium models of differentially rotating polytropes and the collapse of rotating stellar cores, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Equilibrium models of differentially rotating polytropes and the collapse of rotating stellar cores will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1663186