The masses and radii of non-rotating and rotating configurations of pure hadronic stars mixed with selfinteracting fermionic asymmetric dark matter are calculated within the two-fluid formalism of stellar structure equations in general relativity. The Equation of State (EoS) of nuclear matter is obtained from the density dependent M3Y effective nucleon-nucleon interaction. We consider the dark matter particle mass of 1 GeV. The EoS of self-interacting dark matter is taken from two-body repulsive interactions of the scale of strong interactions. We explore the conditions of equal and different rotational frequencies of nuclear matter and dark matter and find that the maximum mass of differentially rotating stars with self-interacting dark matter to be ∼1.94 M with radius ∼10.4 km.

In this work we study the r-mode instability windows and the gravitational wave signatures of neutron stars in the slow rotation approximation using the equation of state obtained from the density dependent M3Y effective interaction. We consider the neutron star matter to be βequilibrated neutron-proton-electron matter at the core with a rigid crust. The fiducial gravitational and viscous timescales, the critical frequencies and the time evolutions of the frequencies and the rates of frequency change are calculated for a range of neutron star masses. We show that the young and hot rotating neutron stars lie in the r-mode instability region. We also emphasize that if the dominant dissipative mechanism of the r-mode is the shear viscosity along the boundary layer of the crust-core interface, then the neutron stars with low L value lie in the r-mode instability region and hence emit gravitational radiation.

In the original publication of the article on p. 3 first paragraph a v was not correctly displayed. Correct form of the paragraph:The calculations are performed using the values of the saturation density ρ 0 = 0.1533 fm −3 [42] and the saturation energy per nucleon 0 = −15.26 MeV [43] for the SNM obtained from the coefficient of the volume term of the Bethe-Weizsäcker mass formula which is evaluated by fitting the recent experimental and estimated atomic mass excesses from the Audi-Wapstra-Thibault atomic mass table [44] by minimizing the mean square deviation incorporating correction for the electronic binding energy [45]. In a similar recent work, addressing the surface symmetry energy term, the Wigner term, the shell correction and the proton form factor correction to the Coulomb energy, the a v turns out to be 15.4496 MeV and when the A 0 and A 1/3 terms are alsoThe online version of the original article can be found under doi:10.1140/epjc/s10052-017-5006-3. included it becomes 14.8497 MeV [46]. Using the usual values of α = 0.005 MeV −1 for the parameter of the energy dependence of the zero range potential and n = 2/3, the values obtained for the constants of density dependence C and β and the SNM incompressibility K ∞ are 2.2497, 1.5934 fm 2 and 274.7 MeV, respectively. The saturation energy per nucleon is the volume energy coefficient and the value of −15.26 ± 0.52 MeV covers, more or less, the entire range of values obtained for a v for which now we have the values of C = 2.2497 ± 0.0420, β = 1.5934 ± 0.0085 fm 2 and the SNM incompressibility K ∞ = 274.7 ± 7.4 MeV.The original article has been corrected.