EPJ Web of Conferences
Volume 109, 2016The 13th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG2015)
|Number of page(s)||6|
|Section||Neutron Star and High Density Matter|
|Published online||12 February 2016|
Shedding Light on the EOS-Gravity Degeneracy and Constraining the Nuclear Symmetry Energy from the Gravitational Binding Energy of Neutron Stars
1 College of Material Science and Technology, Nanjing University of Aeronautics and Astronautics, Nanjing 210016, China
2 Department of Physics and Astronomy, Texas A&M University-Commerce, Commerce, TX 75429, USA
3 Center for Exploration of Energy and Matter, Indiana University, Bloomington IN 47408, USA
Published online: 12 February 2016
A thorough understanding of properties of neutron stars requires both a reliable knowledge of the equation of state (EOS) of super-dense nuclear matter and the strong-field gravity theories simultaneously. To provide information that may help break this EOS-gravity degeneracy, we investigate effects of nuclear symmetry energy on the gravitational binding energy of neutron stars within GR and the scalar-tensor subset of alternative gravity models. We focus on effects of the slope L of nuclear symmetry energy at saturation density and the high-density behavior of nuclear symmetry energy. We find that the variation of either the density slope L or the high-density behavior of nuclear symmetry energy leads to large changes in the binding energy of neutron stars. The difference in predictions using the GR and the scalar-tensor theory appears only for massive neutron stars, and even then is significantly smaller than the difference resulting from variations in the symmetry energy.
© Owned by the authors, published by EDP Sciences, 2016
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