Astronomy and Astrophysics – Astrophysics
Scientific paper
2003-02-20
Astrophys.J.595:352-364,2002
Astronomy and Astrophysics
Astrophysics
15 pages, 19 figures included, uses emulateapj5.sty (included). Accepted for publication in The Astrophysical Journal
Scientific paper
10.1086/377334
We investigate the dynamical instability of the one-armed spiral m=1 mode in differentially rotating stars by means of 3+1 hydrodynamical simulations in Newtonian gravitation. We find that both a soft equation of state and a high degree of differential rotation in the equilibrium star are necessary to excite a dynamical m=1 mode as the dominant instability at small values of the ratio of rotational kinetic to potential energy, T/|W|. We find that this spiral mode propagates outward from its point of origin near the maximum density at the center to the surface over several central orbital periods. An unstable m=1 mode triggers a secondary m=2 bar mode of smaller amplitude, and the bar mode can excite gravitational waves. As the spiral mode propagates to the surface it weakens, simultaneously damping the emitted gravitational wave signal. This behavior is in contrast to waves triggered by a dynamical m=2 bar instability, which persist for many rotation periods and decay only after a radiation-reaction damping timescale.
Baumgarte Thomas W.
Saijo Motoyuki
Shapiro Stuart L.
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