The Critical Rotation of Strange Stars and Rapidly Rotating Pulsars
arXiv:astro-ph/0305034 · doi:10.1086/374370
Abstract
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.
10pages,5figures
References in corpus (25)
- A new class of unstable modes of rotating relativistic stars
- Gravitational waves from hot young rapidly rotating neutron stars
- Gravitational Radiation Instability in Hot Young Neutron Stars
- Axial instability of rotating relativistic stars
- Gravitational radiation limit on the spin of young neutron stars
- On the relevance of the r-mode instability for accreting neutron stars and white dwarfs
- Probing strange stars and color superconductivity by r-mode instabilities in millisecond pulsars
- On the dynamics of superfluid neutron star cores
- R-Mode Oscillations in Rotating Magnetic Neutron Stars
- R-mode runaway and rapidly rotating neutron stars
- Viscous Boundary Layer Damping of R-Modes in Neutron Stars
- Prospects of Detecting Baryon and Quark Superfluidity from Cooling Neutron Stars
- Strange stars as persistent sources of gravitational waves
- How to identify a Strange Star
- R-Modes in Superfluid Neutron Stars
- Medium effects in strange quark matter and strange stars
- R-Mode Oscillations and Spindown of Young Rotating Magnetic Neutron Stars
- Non-Linear Evolution of the r-Modes in Neutron Stars
- Second-order rotational effects on the r-modes of neutron stars
- Effect of a neutron-star crust on the r-mode instability
- Braaten-Pisarski Method at Finite Chemical Potential
- Quasi-toroidal oscillations in rotating relativistic stars
- Collective fermionic excitations in systems with a large chemical potential
- Magnetic effects on the viscous boundary layer damping of the r-modes in neutron stars
- Vorticity affects the stability of neutron stars
Cited by in corpus (5)
- Running coupling constant from lattice data and bulk viscosity of strange quark matter
- Bulk viscosity of strange quark matter in density-dependent quark mass model and dissipation of r-modes in strange stars
- Bulk viscosity of Mixed nucleon-hyperon-quark Matter in Neutron stars
- R-mode instability of strange stars and observations of neutron stars in LMXBs
- Implication of Existence of Hybrid stars and Theoretical Expectation of Submillisecond Pulsars