{ "id": "0912.3052", "version": "v1", "published": "2009-12-16T04:16:33.000Z", "updated": "2009-12-16T04:16:33.000Z", "title": "The role of $r$-mode damping in the thermal evolution of neutron stars", "authors": [ "Shu-Hua Yang", "Xiao-Ping Zheng", "Chun-Mei Pi", "Yun-Wei Yu" ], "comment": "12 pages, 3 figures", "journal": "MNRAS 403, 2007-2011(2010)", "categories": [ "astro-ph.HE" ], "abstract": "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.", "revisions": [ { "version": "v1", "updated": "2009-12-16T04:16:33.000Z" } ], "analyses": { "keywords": [ "neutron stars", "thermal evolution", "mode damping", "second order model", "heating effect" ], "tags": [ "journal article" ], "publication": { "doi": "10.1111/j.1365-2966.2010.16238.x", "journal": "Monthly Notices of the Royal Astronomical Society", "year": 2010, "month": "Apr", "volume": 403, "number": 4, "pages": 2007 }, "note": { "typesetting": "TeX", "pages": 12, "language": "en", "license": "arXiv", "status": "editable", "inspire": 840243, "adsabs": "2010MNRAS.403.2007Y" } } }