Heavy ion collisions with A = 1057: Aspects of nuclear stability and the nuclear equation of state in coalescing neutron-star binary systems

Details Heavy ion collisions with A = 1057: Aspects of nuclear stability and the nuclear equation of state in coalescing neutron-star binary systems Heavy ion collisions with A = 1057: Aspects of nuclear stability and the nuclear equation of state in coalescing neutron-star binary systems

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987honu.symp.....m&link_type=abstract

Presented at the Symposium on Hot Nuclei, College Station, Tex., 7 Dec. 1987

Astronomy and Astrophysics

Astrophysics

Heavy Ions, Neutron Stars, Nuclear Fusion, Particle Collisions, Astrophysics, Binary Stars, Coalescing, Equations Of State, Gravitational Waves, Hydrodynamics, Stability

Scientific paper

The dynamics of the final stages of the coalescence of two neturon stars (such as the binary pulsar PSR 1913+16) is an unsolved problem in astrophysics. Such systems are probably efficient generators of gravitational radiation, and may be significant contributors to heavy-element nucleosynthesis. The input physics for the study of such systems is similar to that required for the study of heavy-ion collision hydrodynamics; e.g., a finite temperature nuclear equation of state, properties of nuclei away from stability, etc. We discuss the development of a relativistic hydrodynamics code in three spatial dimensions for the purpose of studying such neutron-star systems. The properties of the mass-radius relation (determined by the nuclear equation of state) may lead to a proposed mechanism by which hot, highly neutronized matter is ejected from the coalescing stars. This material is photodisintegrated into a free (mostly) neutron gas which may subsequently experience rapid-neutron capture (r-process) nucleosynthesis.

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