Erratum to: Compact bifluid hybrid stars: hadronic matter mixed with self-interacting fermionic asymmetric dark matter

Abstract

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.

Mass-Radius Relationship of Neutron Stars Admixed with Fermionic Asymmetric Dark Matter

“…Moreover, we find that these neutron stars admixed with dark matter typically show characteristics similar to self-bound strange stars in the low mass region. This is because of the very strong two-body repulsive interactions of dark matter which counteracts gravity effectively for low mass region and makes radius much smaller compared to pure neutron star of similar mass [2].…”

“…The EoS of fermionic ADM is obtained by considering the dark matter particles as fermions strongly interacting with each other within the context of vector meson effective field theory. The total energy density and pressure of self-interacting fermionic dark particles is given respectively by [2], Proc. 13th Int.…”