2001
DOI: 10.1103/physrevlett.86.1384
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Comment on “Gravitational Radiation Instability in Hot Young Neutron Stars”

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Cited by 68 publications
(79 citation statements)
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“…For example, it can drive a secular bar instability in rapidly rotating neutron stars, as shown in Newtonian gravitation [1,2] and in general relativity [3]. Viscosity can suppress the r-modes [4,5] and other gravitational-radiation driven instabilities, including the secular bar modes [6]. Viscosity also destroys differential rotation, and this can cause significant changes in the structure and evolution of differentially rotating massive neutron stars.…”
Section: Introductionmentioning
confidence: 99%
“…For example, it can drive a secular bar instability in rapidly rotating neutron stars, as shown in Newtonian gravitation [1,2] and in general relativity [3]. Viscosity can suppress the r-modes [4,5] and other gravitational-radiation driven instabilities, including the secular bar modes [6]. Viscosity also destroys differential rotation, and this can cause significant changes in the structure and evolution of differentially rotating massive neutron stars.…”
Section: Introductionmentioning
confidence: 99%
“…Even if the initial field is weak, fluid motions produced by these oscillations may amplify the magnetic field and eventually distort or suppress the r-modes altogether. (R-modes may also be suppressed by non-linear mode coupling [23] or hyperon bulk viscosity [24]. )…”
Section: Introductionmentioning
confidence: 99%
“…We then obtain (after an approximate algebraic simplification) The third term arises from the bulk viscosity produced by out-of-equilibrium hyperon reactions (which dominate that produced by direct and modified Urca reactions). This has been studied by Jones (2001aJones ( , 2001b and Lindblom & Owen (2002) for normal nuclear matter and by Haensel, Levenfish, & Yakovlev (2002) for superfluids. We employ the results of Lindblom & Owen (2002) for .…”
mentioning
confidence: 99%