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
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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