Abstract
We have calculated total masses and radii of neutron stars from the Tolman-Oppenheimer Volkoff (TOV) equations (form matter in equilibrium in gravitational fields) and different equations of state for neutron-star matter. The calculations are done for different input central densities. We have also obtained pressure and density as a function of distance from the center of the star, the moment of inertia and the surface gravitational redshift as a function of the total mass of the star. The maximum mass M{sub max} is for all equations of state in our calculations given by 1.65M{sub sun} < M{sub max} < 2.43M{sub sun} (where M{sub sun} is the solar mass), which agrees very well with ``experimental`` results. Corresponding radii R are given by 8.8km < R < 12.7km, and a smaller central density will, in general, give a smaller mass and a larger radius. (author). 11 refs, 19 figs, 8 tabs.
Bao, G;
[1]
Oestgaard, E;
[2]
Dybvik, B
[3]
- International Centre for Theoretical Physics, Trieste (Italy)
- Trondheim Univ., Dragvoll (Norway). Physics Inst.
- Trondheim Univ. (Norway). Inst. for Fysikk
Citation Formats
Bao, G, Oestgaard, E, and Dybvik, B.
Equation of state, mass and radius for neutron stars.
IAEA: N. p.,
1993.
Web.
Bao, G, Oestgaard, E, & Dybvik, B.
Equation of state, mass and radius for neutron stars.
IAEA.
Bao, G, Oestgaard, E, and Dybvik, B.
1993.
"Equation of state, mass and radius for neutron stars."
IAEA.
@misc{etde_10144827,
title = {Equation of state, mass and radius for neutron stars}
author = {Bao, G, Oestgaard, E, and Dybvik, B}
abstractNote = {We have calculated total masses and radii of neutron stars from the Tolman-Oppenheimer Volkoff (TOV) equations (form matter in equilibrium in gravitational fields) and different equations of state for neutron-star matter. The calculations are done for different input central densities. We have also obtained pressure and density as a function of distance from the center of the star, the moment of inertia and the surface gravitational redshift as a function of the total mass of the star. The maximum mass M{sub max} is for all equations of state in our calculations given by 1.65M{sub sun} < M{sub max} < 2.43M{sub sun} (where M{sub sun} is the solar mass), which agrees very well with ``experimental`` results. Corresponding radii R are given by 8.8km < R < 12.7km, and a smaller central density will, in general, give a smaller mass and a larger radius. (author). 11 refs, 19 figs, 8 tabs.}
place = {IAEA}
year = {1993}
month = {Feb}
}
title = {Equation of state, mass and radius for neutron stars}
author = {Bao, G, Oestgaard, E, and Dybvik, B}
abstractNote = {We have calculated total masses and radii of neutron stars from the Tolman-Oppenheimer Volkoff (TOV) equations (form matter in equilibrium in gravitational fields) and different equations of state for neutron-star matter. The calculations are done for different input central densities. We have also obtained pressure and density as a function of distance from the center of the star, the moment of inertia and the surface gravitational redshift as a function of the total mass of the star. The maximum mass M{sub max} is for all equations of state in our calculations given by 1.65M{sub sun} < M{sub max} < 2.43M{sub sun} (where M{sub sun} is the solar mass), which agrees very well with ``experimental`` results. Corresponding radii R are given by 8.8km < R < 12.7km, and a smaller central density will, in general, give a smaller mass and a larger radius. (author). 11 refs, 19 figs, 8 tabs.}
place = {IAEA}
year = {1993}
month = {Feb}
}