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

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

2009-12-16

arxiv.org/abs/0912.3052v1

MNRAS 403, 2007-2011(2010)

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

12 pages, 3 figures

Scientific paper

The thermal evolution of neutron stars (NSs) is investigated by coupling with the evolution of $\textit{r}$-mode instability that is described by a second order model.The heating effect due to shear viscous damping of the $\textit{r}$-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 $\textit{r}$-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.

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