Neutron stars and nuclei in the modified relativistic Hartree approximation

M. Prakash, P. J. Ellis, E. K. Heide, S. Rudaz

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We have examined the properties of neutron-rich matter and finite nuclei in the modified relativistic Hartree approximation for several values of the renormalization parameter, μ, around the standard choice of μ equal to the nucleon mass M. Observed neutron-star masses do not effectively constrain the value of μ. However, for finite nuclei the value μ/M = 0.79, suggested by nuclear matter data, provides a good account of the bulk properties with a sigma mass of about 600 MeV. This value of μ/M renders the effective three- and four-body scalar self-couplings to be zero at 60% of equilibrium nuclear matter density. We have also found that the matter part of the exchange diagram has little impact on the bulk properties of neutron stars.

Original languageEnglish (US)
Pages (from-to)583-604
Number of pages22
JournalNuclear Physics, Section A
Issue number3
StatePublished - Aug 8 1994

Bibliographical note

Funding Information:
We thank C.J. Horowitz for giving us a copy of his computerc ode for finite nuclei and for discussions pertaining thereto.W e acknowledgep artial supportf rom the Department of Energy under contracts No. ~E-FG~-~~E~~~32~~~ E”AC~2-~3E~4~10ã nd DE-FG~2-~8~~4~3~Ã. grant for computing time from the Minnesota Supercomputer Institute is gratefully acknowledged.


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