منابع مشابه
Anisotropic convection in rotating proto-neutron stars
We study the conditions for convective instability in rotating, non-magnetic proto–neutron stars. The criteria that determine stability of nascent neutron stars are analogous to the Solberg–Høiland conditions but including the presence of lepton gradients. Our results show that, for standard angular velocity profiles, convectively unstable modes with wave-vectors parallel to the rotation axis a...
متن کاملSurface gravity of neutron stars and strange stars
The upper bound on the value of the surface gravity, gs, for neutron stars with equations of state respecting vsound ≤ c, is derived. This bound is inversely proportional to the maximum allowable mass Mmax, and it reads gs ≤ 1.411× 10 15 (Mmax/M⊙) −1 cm s. It implies an absolute upper bound 7.4× 10 cm s if one uses the 2σ lower bound on the neutron mass measured recently in 4U1700-37, 1.9M⊙. A ...
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Considering the non-Newtonian gravity proposed in grand unification theories, we show that the stability and observed global properties of neutron stars cannot rule out the supersoft nuclear symmetry energies at suprasaturation densities. The degree of possible violation of the inverse-square law of gravity in neutron stars is estimated using an equation of state of neutron-rich nuclear matter ...
متن کاملStrong energy condition in R+R2 gravity.
In this paper, we study Raychaudhuri's equation in the background of R + βR 2 gravity with a phenomenological matter (ρ ∝ a(t) −n). We conclude that even though the Strong Energy Condition (S.E.C.) for Einstein's gravity, which guarantees singularity, is n ≥ 2 for ρ ∝ a(t) −n , a perturbative analysis of Raychaudhuri's equation in the background of R+βR 2 gravity reveals that the big bang singu...
متن کاملSpin and Isospin Asymmetry, Equation of State and Neutron Stars
In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.
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ژورنال
عنوان ژورنال: Physical Review D
سال: 2018
ISSN: 2470-0010,2470-0029
DOI: 10.1103/physrevd.97.124009