The r-mode instability windows of hybrid stars |
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| Institution: | 1. Dept. of Physics, Aristotle University of Thessaloniki, 55124 Thessaloniki, Greece;2. Institut für Theoretische Physik, Universität Giessen, D-35392 Giessen, Germany;3. GSI Helmholtzzentrum für Schwerionenforschung, D-64291 Darmstadt, Germany;1. Department of Physics, Princeton University, Princeton, NJ 08544, USA;2. eXtreme Gravity Institute, Department of Physics, Montana State University, Bozeman, MT 59717, USA;1. Department of Astronomy, Xiamen University, Xiamen 361005, China;2. Institute for Theoretical Physics, Frankfurt am Main 60438, Germany;3. Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, Potsdam-Golm, 14476, Germany;4. Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China;5. School of Physics, Nankai University, Tianjin 300071, China;6. Strangeness Nuclear Physics Laboratory, RIKEN Nishina Center, Wako, 351-0198, Japan;7. School of Information Science and Engineering, Zhejiang University Ningbo Institute of Technology, Ningbo 315100, China;8. Advanced Science Research Center, Japan Atomic Energy Research Institute, Tokai, Ibaraki 319-1195, Japan |
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| Abstract: | Taking into account the peculiar properties of hybrid stars, stars containing both a core of strange quark matter and the solid crust of a neutron star, and employing a fully self-consistent second-order correction technique, we study the time scale of bulk viscosity dissipation at the low temperature limit (T < 109 K) and with this time scale we calculate the critical spin frequency of the hybrid star. It is found that its minimal value is 704.42 Hz (corresponding to a pulse period of 1.42 ms). When this is compared with the periods of neutron and strange stars, a better interpretation of the observational data is obtained. |
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