A two-density neutron star model with continuity of density

Details A two-density neutron star model with continuity of density A two-density neutron star model with continuity of density

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.167...41n&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 167, no. 1, May 1990, p. 41-53.

Statistics

Computation

Neutron Stars, Stellar Models, Stellar Physics, Computational Astrophysics, Stellar Cores, Stellar Envelopes

Scientific paper

Tolman's (1939) V solution has found wide application to the redshift problems in astrophysics, but it has a drawback in that there is a singularity at the center. A two-density model is developed with a parabolic density distribution in the core and e exp v proportional to r exp 2n in the envelope. The most distinctive feature of the model is a continuity of all four variables at the boundary. In other analytic core-envelope models the continuity of only three variables is possible. This two-density structure has been used to model neutron stars and their masses, sizes, and redshifts.

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