Tolman–Oppenheimer–Volkoff (TOV) Stars
نویسنده
چکیده
We present a set of lecture notes for modeling stellar structure in regimes where general relativistic effects become important, such as for neutron stars. The framework draws directly from solving the Einstein equation for a spherically symmetric star in static equilibrium in terms of energy density, pressure, and a term like the gravitational potential. The equation is presented as a somewhat intuitive extension of what was covered regarding stars in hydrostatic equilibrium. Furthermore, we numerically solve the TOV equation in the case of a piecewise polytropic equation of state to find a theoretical upper limit on the mass of neutron stars. For the model considered we find a maximum mass of 2.122 M , in agreement with the currently accepted range of 1.44 to 3 M for neutron stars.
منابع مشابه
From Quark Stars to Hybrid Stars
We show the possible existence of compact stars having a surface composed of a mixed phase of quarks and hadrons. This scenario can be realized both for self-bound stars, satisfying the so-called Witten-Bodmer hypothesis, and for gravitationally bound stars. This class of solutions of the Tolman-Oppenheimer-Volkoff equation can be obtained in all the models we discuss, within a physically accep...
متن کاملThe thermodynamics of collapsars
This article argues that there is a consistent description of gravitationally collapsed bodies, including neutron stars above the Tolman-Oppenheimer-Volkoff mass and also supermassive galactic centres, according to which collapse stops before the object reaches its gravitational radius, the density reaching a maximum close to the surface and then decreasing towards the centre. Models for such s...
متن کاملHolographic neutron stars
We construct in the context of the AdS/CFT correspondence degenerate composite operators in the conformal field theory that are holographically dual to degenerate stars in anti de Sitter space. We calculate the effect of the gravitational back-reaction using the Tolman-Oppenheimer-Volkoff equations, and determine the ”Chandrasekhar limit” beyond which the star undergoes gravitational collapse t...
متن کاملPhase Transition and Hybrid Star in a Su(2) Chiral Sigma Model
We use a modified SU(2) chiral sigma model to study nuclear matter at high density using mean field approach. We also study the phase transition of nuclear matter to quark matter in the interior of highly dense neutron stars. Stable solutions of Tolman-Oppenheimer-Volkoff equations representing hybrid stars are obtained with a maximum mass of 1.69M ⊙ , radii around 9.3 kms and a quark matter co...
متن کاملar X iv : n uc l - th / 0 30 70 57 v 1 1 3 Ju l 2 00 3 SU ( 2 ) CHIRAL SIGMA MODEL STUDY OF PHASE TRANSITION IN HYBRID STARS
We use a modified SU(2) chiral sigma model to study nuclear matter component and simple bag model for quark matter constituting a neutron star. We also study the phase transition of nuclear matter to quark matter with the mixed phase characterized by two conserved charges in the interior of highly dense neutron stars. Stable solutions of Tolman-Oppenheimer-Volkoff equations representing hybrid ...
متن کامل