Probing strange stars and color superconductivity by r-mode instabilities in millisecond pulsars

Physical Review Letters

Volumn 85, Issue 1, 2000, Pages 10-13

  Madsen, Jes ^a  

^a AARHUS UNIVERSITY   (Denmark)

Author keywords

[No Author keywords available]

Indexed keywords

ELECTRON TRANSPORT PROPERTIES; ELECTRONIC DENSITY OF STATES; ENERGY GAP; FREQUENCIES; NEUTRONS; ROTATION; STABILITY; SUPERCONDUCTIVITY; THERMAL EFFECTS;

MILLISECOND PULSARS; NORMAL MATTER QUAR PHASE; TWO FLAVOR COLOR SUPERCONDUCTIVITY;

CHARGED PARTICLES;

EID: 0034229341     PISSN: 00319007     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevLett.85.10     Document Type: Article

References (34)

1. N. Andersson, Astrophys. J. 502, 708 (1998).
2. J. L. Friedman and S. M. Morsink, Astrophys. J. 502, 714 (1998).
3. L. Lindblom, B. J. Owen, and S. M. Morsink, Phys. Rev. Lett. 80, 4843 (1998).
4. B. J. Owen et al., Phys. Rev. D 58, 084020 (1998).
5. J. Madsen, Phys. Rev. Lett. 81, 3311 (1998).
6. Y. Kojima, Mon. Not. R. Astron. Soc. 293, 423 (1998).
7. N. Andersson, K. D. Kokkotas, and B. F. Schutz, Astrophys. J. 510, 846 (1999).
8. N. Andersson, K. D. Kokkotas, and N. Stergioulas, Astrophys. J. 516, 307 (1999).
9. Y. Levin, Astrophys. J. 517, 328 (1999).
10. K. H. Lockitch and J. L. Friedman, Astrophys. J. 521, 764 (1999).
11. K. D. Kokkotas and N. Stergioulas, Astron. Astrophys. 341, 110 (1999).
12. L. Lindblom, G. Mendell, and B. J. Owen, Phys. Rev. D 60, 064006 (1999).
13. Y. Kojima and M. Hosonuma, Astrophys. J. 520, 788 (1999).
14. V. Rezania and R. Maartens, Phys. Rev. Lett. 84, 2560 (2000).
15. V. Rezania and M. Jahan-Miri, astro-ph/9910515.
16. L. Lindblom and G. Mendell, Phys. Rev. D 61, 104003 (2000).
17. S. Yoshida et al., astro-ph/9910532.
18. L. Bildsten and G. Ushomirsky, Astrophys. J. 529, L33 (2000); see also N. Andersson et al., ibid. 534, L75 (2000).
19. L. Bildsten and G. Ushomirsky, Astrophys. J. 529, L33 (2000); see also N. Andersson et al., ibid. 534, L75 (2000).
20. L. Rezzolla, F. K. Lamb, and S. L. Shapiro, Astrophys. J. 531, L141 (2000).
21. W. C. G. Ho and D. Lai, astro-ph/9912296.
22. For reviews and extensive references on CFL and 2SC, see K. Rajagopal, hep-ph/9908360; F. Wilczek, hep-ph/ 9908480; T. Schäfer, nucl-th/9911017. For applications to compact star magnetic fields and cooling, see M. Alford, J. Berges, and K. Rajagopal, Nucl. Phys. B571, 269 (2000); D. Blaschke, D. M. Sedrakian, and K. M. Shahabasyan, Astron. Astrophys. 350, L47 (1999); D. Blaschke, T. Klähn, and D. N. Voskresensky, Astrophys. J. 533, 406 (2000).
23. For reviews and extensive references on CFL and 2SC, see K. Rajagopal, hep-ph/9908360; F. Wilczek, hep-ph/ 9908480; T. Schäfer, nucl-th/9911017. For applications to compact star magnetic fields and cooling, see M. Alford, J. Berges, and K. Rajagopal, Nucl. Phys. B571, 269 (2000); D. Blaschke, D. M. Sedrakian, and K. M. Shahabasyan, Astron. Astrophys. 350, L47 (1999); D. Blaschke, T. Klähn, and D. N. Voskresensky, Astrophys. J. 533, 406 (2000).
24. For reviews and extensive references on CFL and 2SC, see K. Rajagopal, hep-ph/9908360; F. Wilczek, hep-ph/ 9908480; T. Schäfer, nucl-th/9911017. For applications to compact star magnetic fields and cooling, see M. Alford, J. Berges, and K. Rajagopal, Nucl. Phys. B571, 269 (2000); D. Blaschke, D. M. Sedrakian, and K. M. Shahabasyan, Astron. Astrophys. 350, L47 (1999); D. Blaschke, T. Klähn, and D. N. Voskresensky, Astrophys. J. 533, 406 (2000).
25. For reviews and extensive references on CFL and 2SC, see K. Rajagopal, hep-ph/9908360; F. Wilczek, hep-ph/ 9908480; T. Schäfer, nucl-th/9911017. For applications to compact star magnetic fields and cooling, see M. Alford, J. Berges, and K. Rajagopal, Nucl. Phys. B571, 269 (2000); D. Blaschke, D. M. Sedrakian, and K. M. Shahabasyan, Astron. Astrophys. 350, L47 (1999); D. Blaschke, T. Klähn, and D. N. Voskresensky, Astrophys. J. 533, 406 (2000).
26. For reviews and extensive references on CFL and 2SC, see K. Rajagopal, hep-ph/9908360; F. Wilczek, hep-ph/ 9908480; T. Schäfer, nucl-th/9911017. For applications to compact star magnetic fields and cooling, see M. Alford, J. Berges, and K. Rajagopal, Nucl. Phys. B571, 269 (2000); D. Blaschke, D. M. Sedrakian, and K. M. Shahabasyan, Astron. Astrophys. 350, L47 (1999); D. Blaschke, T. Klähn, and D. N. Voskresensky, Astrophys. J. 533, 406 (2000).
27. For reviews and extensive references on CFL and 2SC, see K. Rajagopal, hep-ph/9908360; F. Wilczek, hep-ph/ 9908480; T. Schäfer, nucl-th/9911017. For applications to compact star magnetic fields and cooling, see M. Alford, J. Berges, and K. Rajagopal, Nucl. Phys. B571, 269 (2000); D. Blaschke, D. M. Sedrakian, and K. M. Shahabasyan, Astron. Astrophys. 350, L47 (1999); D. Blaschke, T. Klähn, and D. N. Voskresensky, Astrophys. J. 533, 406 (2000).
28. C. Alcock, E. Farhi, and A. Olinto, Astrophys. J. 310, 261 (1986); C. Kettner, F. Weber, M. K. Weigel, and N. K. Glendenning, Phys. Rev. D 51, 1440 (1995).
29. C. Alcock, E. Farhi, and A. Olinto, Astrophys. J. 310, 261 (1986); C. Kettner, F. Weber, M. K. Weigel, and N. K. Glendenning, Phys. Rev. D 51, 1440 (1995).
30. Viscosity due to magnetic fields and vorticity discussed in [14,19,20] would not change the main conclusions of the present study.
31. H. Heiselberg and C. J. Pethick, Phys. Rev. D 48, 2916 (1993).
32. J. Madsen, Phys. Rev. D 46, 3290 (1992).
33. If the electron fraction is very low, cooling may be slower than assumed here, cf. C. Schaab, B. Hermann, F. Weber, and M. K. Weigel, Astrophys. J. 480, L111 (1997).
34. -3; not quite neutron drip density, cf. Q. D. Huang and T. Lu, Astron. Astrophys. 325, 189 (1997).