Skip to main content
. 2003 Jun 16;6(1):3. doi: 10.12942/lrr-2003-3

Figure 15.

Figure 15

Density contours and velocity flow for a neutron star model that has developed spiral arms, due to the dynamical bar-mode instability. The computation was done in full General Relativity. (Figure 4 of Shibata, Baumgarte, and Shapiro [ 274 ]; used with permission).