Nuclear Science and Techniques

《核技术》(英文版) ISSN 1001-8042 CN 31-1559/TL     2019 Impact factor 1.556

Nuclear Science and Techniques ›› 2018, Vol. 29 ›› Issue (12): 178 doi: 10.1007/s41365-018-0515-9

Special Issue: Special Section on International Workshop on Nuclear Dynamics in Heavy-Ion Reaction (IWND2018)

• Special Section on International Workshop on Nuclear Dynamics in Heavy-Ion Reaction (IWND2018) • Previous Articles     Next Articles

Astrophysical constraints on a parametric equation of state for neutron-rich nucleonic matter

Nai-Bo Zhang 1,2 • Bao-An Li 2   

  1. 1 Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University, Weihai 264209, China
    2 Department of Physics and Astronomy, Texas A&M University-Commerce, Commerce, TX 75429, USA
  • Contact: Bao-An Li E-mail:Bao-An.Li@Tamuc.edu
  • Supported by:

    NBZ was supported in part by the China Scholarship Council. BAL acknowledges the U.S. Department of Energy, Office of Science, under Award Number DE-SC0013702, the CUSTIPEN (China-U.S. Theory Institute for Physics with Exotic Nuclei) under the U.S. Department of Energy Grant No. DE-SC0009971 and the National Natural Science Foundation of China under Grant No. 11320101004.

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Nai-Bo Zhang, Bao-An Li. Astrophysical constraints on a parametric equation of state for neutron-rich nucleonic matter.Nuclear Science and Techniques, 2018, 29(12): 178     doi: 10.1007/s41365-018-0515-9

Abstract:

Extracting the equation of state (EOS) and symmetry energy of dense neutron-rich matter from astrophysical observations is a long-standing goal of nuclear astrophysics. To facilitate the realization of this goal, the feasibility of using an explicitly isospin-dependent parametric EOS for neutron star matter was investigated recently in [1–3]. In this contribution, in addition to outlining the model framework and summarizing the most important findings from [1–3], we report a few new results regarding constraining parameters characterizing the highdensity behavior of nuclear symmetry energy. In particular, the constraints on the pressure of neutron star matter extracted from combining the X-ray observations of the neutron star radius, the minimum–maximum mass M =2.01 M, and causality condition agree very well with those extracted from analyzing the tidal deformability data by the LIGO + Virgo Collaborations. The limitations of using the radius and/or tidal deformability of neutron stars to constrain the high-density nuclear symmetry energy are discussed.

Key words: Neutron star, Equation of state, Symmetry energy