SUMMARY AND FUTURE DIRECTIONS
- f-Mode Instabilities
- even at large T/|W|, the growth times for f-mode
secular instabilities are long
---> instability sets in through
a dynamic bar-like mode
- Initial Angular Momentum Distribution
- stellar cores are supported primarily by relativistic degenerate
e-'s
---> secular instability sets in for T/|W| as small as
0.03, with only a weak dependence on compressiblity
- Off-Center Density Maxima
- Shibata, Karino, & Eriguchi (2001) find that
dynamic bar mode instabilities set in
for T/|W| as low as ~0.04
- even at large T/|W|, the growth times for f-mode
secular instabilities are long
---> instability sets in through a dynamic bar-like mode
- stellar cores are supported primarily by relativistic degenerate
e-'s
---> secular instability sets in for T/|W| as small as 0.03, with only a weak dependence on compressiblity
- Shibata, Karino, & Eriguchi (2001) find that dynamic bar mode instabilities set in for T/|W| as low as ~0.04