Simulations of non-axisymmetric rotational core collapse

Details Simulations of non-axisymmetric rotational core collapse Simulations of non-axisymmetric rotational core collapse

1997-11-11

arxiv.org/abs/astro-ph/9711122v1

Astronomy and Astrophysics

Astrophysics

17 pages including all figures. submitted to A&A

Scientific paper

We report on the first three-dimensional hydrodynamic simulations of secular and dynamical non-axisymmetric instabilities in collapsing, rapidly rotating stellar cores which extend well beyond core bounce. The resulting gravitational radiation has been calculated using the quadrupole approximation. We find that secular instabilities do not occur during the simulated time interval of several 10 ms. Models which become dynamically unstable during core collapse show a strong nonlinear growth of non-axisymmetric instabilities. Both random and coherent large scale initial perturbations eventually give rise to a dominant bar-like deformation ($\exp(\pm im\phi$) with $m=2$). In spite of the pronounced tri-axial deformation of certain parts of the core no considerable enhancement of the gravitational radiation is found. This is due to the fact that rapidly rotating cores re-expand after core bounce on a dynamical time scale before non-axisymmetric instabilities enter the nonlinear regime. Hence, when the core becomes tri-axial, it is no longer very compact.

Affiliated with

Also associated with

No associations

Rating

Simulations of non-axisymmetric rotational core collapse 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 Simulations of non-axisymmetric rotational core collapse, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Simulations of non-axisymmetric rotational core collapse will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-200807