Properties of the neutron gas and application to neutron stars

Details Properties of the neutron gas and application to neutron stars Properties of the neutron gas and application to neutron stars

Jul 1971

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971nupha.170....1b&link_type=abstract

Nuclear Physics A, Volume 170, Issue 1, p. 1-11.

Physics

Nuclear Physics

11

Scientific paper

The binding energy of the neutron gas is calculated in Brueckner theory with Ingber's potential which is derived from meson theory. Allowance is then made for the reduction of the pressure due to protons, electrons, mucns, and pions. Reservations must be made even at nuclear matter densities due to the uncertainty in the N-π - and N-Σ- interaction. The resulting equation of state is used to calculate the structure of neutron stars with central densities up to 1015 g/cm3. (A mass of 0.62 Msolar is found at 1015 g/cm3.) It is not possible, however, to determine the maximum neutron star mass, because the central density would exceed 1015 g/cm3, beyond which non-relativistic many-body calculations break down.

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