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R-modes are well known quasi-toroidal oscillations in rotating fluids that happen because of the Coriolis effect [1]. These modes are driven instable by gravitational radiation reactance via the Chandrasekhar-Friedman-Schutz (CFS) mechanism and can increase toroidal magnetic field by inducing differential rotation in neutron stars [2]. The bulk viscosity is the basic dissipation mechanism at high temperature and the shear viscosity is the dominant mechanism at low temperature [3].
In this paper, we study r-mode instability windows and present the calculation of critical angular velocity Ωc [4]. We have used the microscopic lowest order variational (LOCV) method to extract the EOS by employing the realistic nucleon-nucleon interaction [5][6].
[1] B. Haskell, arXiv:1509.04370 [astro-ph.HE] (2015)
[2] Chandrasekhar, S., Phys. Rev. Lett. 24, 611{614 (1970).
[3] A. Idrisy, Benjamin J. Owen, and David. Jones, Phys. Rev. D 91, 024001 (2015)
[4] K.D. Kokkotas, N. Stergioulas arxiv:astro-ph/9805297 (1998)
[5] Z Asadi Aghbolaghi, M Bigdeli, Journal of Physics G: Nuclear and Particle Physics, 065101(2018)
[6] S Goudarzi, HR Moshfegh, PHYSICAL REVIEW C, vol 91, 054320,2015
