Extreme relativistic model for neutron stars and pulsars

Details Extreme relativistic model for neutron stars and pulsars Extreme relativistic model for neutron stars and pulsars

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..90..117d&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 90, no. 1, Feb. 1983, p. 117-126. Research supported by the University Gra

Astronomy and Astrophysics

Astrophysics

2

Neutron Stars, Pulsars, Relativistic Plasmas, Stellar Models, Drag, Magnetohydrodynamic Stability, Moments Of Inertia, Red Shift, Spherical Plasmas, Stellar Gravitation, Stellar Mass, Stellar Oscillations, Stellar Rotation

Scientific paper

Exact solutions are obtained for a massive fluid sphere under the extreme causality condition (dP/d-rho) = 1. It is found that these structures are pulsationally stable for a surface to central density ratio greater than 0.30. Taking the surface density as 2 x 10 to the 14th g/cu cm, the maximum mass of the resulting neutron star is 4.8 solar masses and the size is 20.1 km. The maximum surface redshift for a pulsationally stable structure is 0.75; the corresponding central redshift is 3.40. These structures are gravitationally bound and have a maximum binding energy per unit rest mass of 0.25 at a surface to central density ratio of about 0.40. The differential drag and moment of inertia of a neutron star based on this model are shown. The mass of the Crab pulsar based on this extreme relativistic equation of state is 0.4, 0.5, or 2 solar masses for the three different mechanisms of energy loss which are considered.

Affiliated with

Also associated with

No associations

Rating

Extreme relativistic model for neutron stars and pulsars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Extreme relativistic model for neutron stars and pulsars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Extreme relativistic model for neutron stars and pulsars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1305480