Viscous Damping of r-Modes in Hybrid and Quark Stars(Dense QCD Matter,New Frontiers in QCD 2008-Fundamental Problems in Hot and/or Dense Matter-)

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概要

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• Complementary to the interest in the naturally low viscosity of quark matter at high temperature generated by heavy-ion collisions, the viscosity of quark matter at high density and low temperature is relevant for neutron stars. r-mode oscillations, which cause the star to lose rotational energy via the emission of gravitational waves, are damped by the bulk and shear viscosities of matter. Because of the large viscosity of quark matter relative to hadronic matter, the presence of quark matter in neutron stars increases the amount of viscous damping and makes γ-modes more stable. γ-modes also tend to be more stable in strange quark stars for the same reason. Thus the presence of quarks in dense matter may imply that γ-modes do not contribute to the spin-down of compact objects.

• 理論物理学刊行会の論文
• 2008-10-15

著者

• Steiner Andrew

  Joint Institude For Nuclear Astrophysics National Superconducting Cyclotron Laboratory And The Depar

• STEINER Andrew

  Joint Institude for Nuclear Astrophysics, National Superconducting Cyclotron Laboratory, and the Department of Physics and Astronomy, Michigan State University

関連論文

• Viscous Damping of r-Modes in Hybrid and Quark Stars(Dense QCD Matter,New Frontiers in QCD 2008-Fundamental Problems in Hot and/or Dense Matter-)

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