Journal Article

The role of <i>r</i>-mode damping in the thermal evolution of neutron stars

Shu-Hua Yang, Xiao-Ping Zheng, Chun-Mei Pi and Yun-Wei Yu

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 403, issue 4, pages 2007-2011
Published in print April 2010 | ISSN: 0035-8711
Published online April 2010 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2010.16238.x
The role of r-mode damping in the thermal evolution of neutron stars

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

Keywords: dense matter; stars: evolution; stars: neutron

Journal Article.  3371 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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