| Issue |
EPJ Web of Conferences
Volume 109, 2016
The 13th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG2015)
|
|
|---|---|---|
| Article Number | 07001 | |
| Number of page(s) | 8 | |
| Section | Neutron Star and High Density Matter | |
| DOI | https://doi.org/10.1051/epjconf/201610907001 | |
| Published online | 12 February 2016 | |
https://doi.org/10.1051/epjconf/201610907001
Neutron Star Physics and EOS
Department of Physics & Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA
a e-mail: James.Lattimer@Stonybrook.edu
Published online: 12 February 2016
Neutron stars are important because measurement of their masses and radii will determine the dense matter equation of state. They will constrain the nuclear matter symmetry energy, which controls the neutron star matter pressure and the interior composition, and will influence the interpretation of nuclear experiments. Astrophysical observations include pulsar timing, X-ray bursts, quiescent low-mass X-ray binaries, pulse profiles from millisecond pulsars, neutrino observations from gravitational collapse supernovae,and gravitational radiation from compact object mergers. These observations will also constrain the neutron star interior, including the properties of superfluidity there, and determine the existence of a possible QCD phase transition.
© Owned by the authors, published by EDP Sciences, 2016
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