The Critical Rotation of Strange Stars and Rapidly Rotating Pulsars

Details The Critical Rotation of Strange Stars and Rapidly Rotating Pulsars The Critical Rotation of Strange Stars and Rapidly Rotating Pulsars

2003-05-02

arxiv.org/abs/astro-ph/0305034v1

Astrophys.J.585:L135-L138,2003

Astronomy and Astrophysics

Astrophysics

10pages,5figures

Scientific paper

10.1086/374370

We utilize the bulk viscosity of interacting strange quark matter to reevaluate the damping time scale. The presence of medium effect of bulk viscosity leads to a stronger damping of r-modes, which can be over an order of magnitude for realistic parameters. We find that the r-mode instability window is narrowed due to the medium effect, and hence when a pulsar reaches the instability window it will only slow down by gravitational wave emission to a period of 1.78msec instead of 2.5msec given by early estimate. As a theoretical upper rotation limit of pulsars, the period of 1.78msec is very close to the two most rapidly spinning pulsars known, with periods of about 1.6msec.

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