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r-Mode Runaway and Rapidly Rotating Neutron Stars.
| Content Provider | Semantic Scholar |
|---|---|
| Author | Andersson, C. Jones Kokkotas Stergioulas |
| Copyright Year | 2000 |
| Abstract | We present a simple spin-evolution model that predicts that rapidly rotating accreting neutron stars will be confined mainly to a narrow range of spin frequencies: P=1.5-5 ms. This is in agreement with current observations of neutron stars in both the low-mass X-ray binaries and the millisecond radio pulsars. The main ingredients in the model are (1) the instability of r-modes above a critical spin rate, (2) the thermal runaway that is due to the heat released as viscous damping mechanisms counteract the r-mode growth, and (3) a revised estimate of the strength of the dissipation that is due to the presence of a viscous boundary layer at the base of the crust in an old and relatively cold neutron star. We discuss the gravitational waves that are radiated during the brief r-mode-driven spin-down phase. We also briefly touch on how the new estimates affect the predicted initial spin periods of hot young neutron stars. |
| Starting Page | L75 |
| Ending Page | L78 |
| Page Count | 4 |
| File Format | PDF HTM / HTML |
| Alternate Webpage(s) | http://arxiv.org/pdf/astro-ph/0002114v2.pdf |
| Alternate Webpage(s) | http://arxiv.org/pdf/astro-ph/0002114v1.pdf |
| PubMed reference number | 10790075v1 |
| Volume Number | 534 |
| Issue Number | 1 |
| Journal | The Astrophysical journal |
| Language | English |
| Access Restriction | Open |
| Subject Keyword | Estimated GUCY2C protein, human Neutrons Revision procedure Scab Stars, Celestial |
| Content Type | Text |
| Resource Type | Article |
