Isospin asymmetric nuclear matter and properties of axisymmetric neutron stars

2010/02/28 by Partha Chowdhury, Partha Roy Chowdhury, Abhijit Bhattacharyya +1 · 9 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #High-pressure geophysics and materials #Isospin #Mechanics #Neutron #Neutron star #Nuclear matter #Nuclear physics #Nuclear physics research studies #Nucleon #Nucleosynthesis #Physics #Pulsars and Gravitational Waves Research #Rotational symmetry #Stars #Strange matter #astro-ph.HE #hep-ph #nucl-ex #nucl-th #r-process

paper · pdf · doi:10.1103/physrevc.81.062801

published in Physical Review C 81(6) (American Institute of Physics) · 5 pages, 4 figures

openalex publication_date 2010/06/23 · arxiv created 2011/01/06 · arxiv updated 2011/01/07 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

Pure hadronic compact stars that are above a limiting value (\ensuremath≈1.6M_\ensuremath\bigodot) of their gravitational masses, to which predictions of most of other equations of state are restricted, can be reached from the equation of state (EOS) obtained using the density-dependent M3Y (DDM3Y) effective interaction. This effective interaction is found to be quite successful in providing a unified description of elastic and inelastic scattering, various radioactivities, and nuclear matter properties. We present a systematic study of the properties of pure hadronic compact stars. The \ensuremathβ-equilibrated neutron star matter using this EOS with a thin crust is able to describe highly massive compact stars, such as PSR B1516+02B with a mass M=1.94_\ensuremath-0.19^+0.17M_\ensuremath\bigodot and PSR J0751+1807 with a mass M=2.1\ifmmode±\else\textpm\fi0.2M_\ensuremath\bigodot to a 1\ensuremathσ confidence level.

Citations

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