The role of $r$-mode damping in the thermal evolution of neutron stars

Abstract

The thermal evolution of neutron stars (NSs) is investigated by coupling with the evolution of $\text{r}$-mode instability that is described by a second order model.The heating effect due to shear viscous damping of the $\text{r}$-modes enables us to understand the high temperature of two young pulsars (i.e., PSR B0531+21 and RX J0822-4300) in the framework of the simple $npe$ NS model, without superfluidity or exotic particles.Moreover, the light curves predicted by the model within an acceptable parameter regime may probably cover all of the young and middle-aged pulsars in the $\lg T_s^{\infty }-\lg t$ panel, and an artificially strong $p$ superfluidity invoked in some early works is not needed here. Additionally, by considering the radiative viscous damping of the $\text{r}$-modes, a surprising extra cooling effect is found, which can even exceed the heating effect sometimes although plays an ignorable role in the thermal history.

12 pages, 3 figures

References in corpus (7)

• Cooling of Neutron Stars. Hadronic Model
• The impact of magnetic field on the thermal evolution of neutron stars
• Theory of cooling neutron stars versus observations
• The influence of differential rotation on the detectability of gravitational waves from the r-mode instability
• Thermal evolution of rotating hybrid stars
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Cited by in corpus (5)

• Viscosity of neutron star matter and $r$-modes in rotating pulsars
• Rapid cooling of neutron star in Cassiopeia A and r-mode damping in the core
• R-mode instability of strange stars and observations of neutron stars in LMXBs
• Mechanism of r-mode stability in young rapidly rotating pulsars
• Evolution of newborn rapidly rotating magnetars: effects of r-mode and fall-back accretion