Neutron Matter from Low to High Density

By Stefano Gandolfi, A. Gezerlis, J. Carlson. 2015

137 citations recorded by the source corpus.

Neutron matter is an intriguing nuclear system with multiple connections to other areas of physics. Considerable progress has been made over the last two decades in exploring the properties of pure neutron fluids. Here we begin by reviewing work done to explore the behavior of very low density neutron matter, which forms a strongly paired superfluid and is thus similar to cold Fermi atoms, though at energy scales differing by many orders of magnitude. We then increase the density, discussing work that ties the study of neutron matter with the determination of the properties of neutron-rich nuclei and neutron-star crusts. After this, we review the impact neutron matter at even higher densities has on the mass-radius relation of neutron stars, thereby making contact with astrophysical observations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/28cde98d5a47f6010a31d11339756fc2fe9e6280

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. J. Lattimer
2. I. Tews
3. C. Heinke
4. A. Steiner
5. Armen Sedrakian
6. W. Ho
7. John W. Clark Jr.
8. S. Reddy

In Nuclear and High Energy Physics

1. I. Tews
2. J. Lattimer
3. Armen Sedrakian
4. John W. Clark Jr.
5. S. Reddy
6. A. Ohnishi
7. E. Kolomeitsev
8. A. Steiner

Citations in the corpus

• Superfluidity in nuclear systems and neutron stars (2018, methodology): “The standard Green Function MC (GFMC) method and the simpler variational MC (VMC) procedure sample only spatial configurations [231, 233, 234].”
• Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations (2018, methodology): “…the EOS of PNM has been computed by using different many-body methods with realistic nucleon– nucleon interactions; see, e.g., Hebeler & Schwenk (2010), Gandolfi et al. (2012, 2015), Tews et al. (2013), Hagen et al. (2014), Sammarruca et al. (2015), Lynn et al. (2016), Drischler et al. (2016),…”
• Constraining the mass and radius of neutron stars in globular clusters (2017, background): “…to lower densities: uncertainties are only well-controlled where the Fermi momentum is small enough to employ chiral effective theory or accurate phenomenological interactions calibrated to nuclei (see recent reviews Gandolfi et al. 2015; Hebeler et al. 2015). c© 0000 The Authors ar X iv :1 70 9.”
• Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, methodology): “While it has been suggested before that the UG is lower in energy than PNM, e.g., Carlson et al. (2002, 2012) and Gandolfi et al. (2015), it has so far not been applied to obtain limits on the symmetry energy parameters.”