Anisotropic hydrodynamics, bulk viscosities, and r-modes of strange quark stars with strong magnetic fields

Journal Article · Mon Feb 15 04:00:00 EST 2010 · Physical Review. D, Particles Fields

DOI:https://doi.org/10.1103/PHYSREVD.81.045015· OSTI ID:21409342

Xuguang, Huang ^[1]; Mei, Huang ^[2]; Rischke, Dirk H ^[1]; Sedrakian, Armen ^[3]

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1. Frankfurt Institute for Advanced Studies, D-60438 Frankfurt am Main (Germany)
2. Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039 (China)
3. Institut fuer Theoretische Physik, J. W. Goethe-Universitaet, D-60438 Frankfurt am Main (Germany)

In strong magnetic fields the transport coefficients of strange quark matter become anisotropic. We determine the general form of the complete set of transport coefficients in the presence of a strong magnetic field. By using a local linear response method, we calculate explicitly the bulk viscosities {zeta}{sub perpendicular} and {zeta}{sub ||} transverse and parallel to the B field, respectively, which arise due to the nonleptonic weak processes u+s{r_reversible}u+d. We find that for magnetic fields B<10{sup 17} G, the dependence of {zeta}{sub perpendicular} and {zeta}{sub ||} on the field is weak, and they can be approximated by the bulk viscosity for the zero magnetic field. For fields B>10{sup 18} G, the dependence of both {zeta}{sub perpendicular} and {zeta}{sub ||} on the field is strong, and they exhibit de Haas-van Alphen-type oscillations. With increasing magnetic field, the amplitude of these oscillations increases, which eventually leads to negative {zeta}{sub perpendicular} in some regions of parameter space. We show that the change of sign of {zeta}{sub perpendicular} signals a hydrodynamic instability. As an application, we discuss the effects of the new bulk viscosities on the r-mode instability in rotating strange quark stars. We find that the instability region in strange quark stars is affected when the magnetic fields exceed the value B=10{sup 17} G. For fields which are larger by an order of magnitude, the instability region is significantly enlarged, making magnetized strange stars more susceptible to r-mode instability than their unmagnetized counterparts.

• OSTI ID: 21409342
• Journal Information: Physical Review. D, Particles Fields, Journal Name: Physical Review. D, Particles Fields Journal Issue: 4 Vol. 81; ISSN PRVDAQ; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
AMPLITUDES
ANISOTROPY
ELEMENTARY PARTICLES
FERMIONS
FLUID MECHANICS
HYDRODYNAMICS
INSTABILITY
MAGNETIC FIELDS
MECHANICS
OSCILLATIONS
QUARKS
S QUARKS
STARS
STRANGE PARTICLES
VISCOSITY