Microscopic calculation of the equation of state of nuclear matter and neutron star structure
Stefano Gandolfi1Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USAA. Yu. Illarionov2International School for Advanced Studies, SISSA, Via Beirut 2/4, I-34014 Trieste, ItalyS. Fantoni2International School for Advanced Studies, SISSA, Via Beirut 2/4, I-34014 Trieste, ItalyJoel C. Miller2International School for Advanced Studies, SISSA, Via Beirut 2/4, I-34014 Trieste, ItalyFrancesco Pederiva4Dipartimento di Fisica dell'Università di Trento, via Sommarive 14, I-38123 Povo, Trento, ItalyK. E. Schmidt8Department of Physics, Arizona State University, Tempe, AZ 85287, USA
2010en
ABI
Аннотация
Abstract We present results for neutron star models constructed with a new equation of state for nuclear matter at zero temperature. The ground state is computed using the auxiliary field diffusion Monte Carlo (AFDMC) technique, with nucleons interacting via a semiphenomenological Hamiltonian including a realistic two-body interaction. The effect of many-body forces is included by means of additional density-dependent terms in the Hamiltonian. In this Letter, we compare the properties of the resulting neutron star models with those obtained using other nuclear Hamiltonians, focusing on the relations between mass and radius, and between the gravitational mass and the baryon number.
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