Abstract.
We demonstrate that stability of r-modes in young rapidly rotating pulsars might be explained if one takes into account strong medium modifications of the nucleon-nucleon interaction because of the softening of pionic degrees of freedom in dense nucleon matter. Presence of the efficient direct Urca processes is not required. Within our model the most rapidly rotating observed young pulsar PSR J0537-6910 should have mass \( \geq 1.8M_{\odot}\).
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References
P. Chatterjee, L. Hernquist, Astrophys. J. 543, 368 (2000)
F.E. Marshall et al., Astrophys. J. 603, 682 (2004)
N. Andersson, Astrophys. J. 502, 708 (1998)
J.L. Friedman, S.M. Morsink, Astrophys. J. 502, 714 (1998)
N. Andersson, K.D. Kokkotas, Int. J. Mod. Phys. D 10, 381 (2001)
L. Lindblom et al., Phys. Rev. Lett. 80, 4843 (1998)
D. Blaschke et al., Phys. Rev. C 88, 065805 (2013)
P.S. Shternin, D.G. Yakovlev, Phys. Rev. D 78, 063006 (2008)
E. Flowers, N. Itoh, Astrophys. J. 230, 847 (1979)
A.B. Migdal et al., Phys. Rep. 192, 179 (1990)
D.N. Voskresensky, A.V. Senatorov, Sov. Phys. JETP 63, 885 (1986)
A.V. Senatorov, D.N. Voskresensky, Phys. Lett. B 184, 119 (1987)
C. Schaab et al., Astron. Astrophys. 321, 591 (1997)
D.N. Voskresensky, Lect. Notes Phys. 578, 467 (2001)
D. Blaschke et al., Astron. Astrophys. 424, 979 (2004)
H. Grigorian, D.N. Voskresensky, Astron. Astrophys. 444, 913 (2005)
D. Blaschke et al., Phys. Rev. C 85, 022802 (2012)
A. Akmal et al., Phys. Rev. C 58, 1804 (1998)
P. Demorest et al., Nature 467, 1081 (2010)
J. Antoniadis et al., Science 340, 6131 (2013)
P. Haensel, A.Y. Potekhin, Astron. Astrophys. 428, 191 (2004)
B.L. Friman, O.V. Maxwell, Astrophys. J. 232, 541 (1979)
A.B. Migdal, Theory of Finite Fermi Systems and Properties of Atomic Nuclei (Wiley and Sons, New York, 1967)
A. Schwenk, B. Friman, Phys. Rev. Lett. 92, 082501 (2004)
D. Page et al., Nucl. Phys. A 777, 497 (2006)
R.F. Sawyer, Phys. Rev. D 39, 3804 (1989)
P. Haensel et al., Astron. Astrophys. 372, 130 (2001)
B.A. Sa’d, J. Schaffner-Bielich, arXiv:0908.4190
S.-H. Yang et al., Phys. Lett. B 683, 255 (2010)
S.-H. Yang et al., Mon. Not. R. Astron. Soc. 403, 2007 (2010)
C. Cutler, L. Lindblom, Astrophys. J. 314, 234 (1987)
M.G. Alford, K. Schwenzer, Astrophys. J. 781, 26 (2014)
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Kolomeitsev, E.E., Voskresensky, D.N. Mechanism of r-mode stability in young rapidly rotating pulsars. Eur. Phys. J. A 50, 180 (2014). https://doi.org/10.1140/epja/i2014-14180-0
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DOI: https://doi.org/10.1140/epja/i2014-14180-0