Maximum mass of neutron stars

By Hans-Josef Schulze, A. Polls, À. Ramos, Isaac Vidaña. 2006

163 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/2be9b5e5d42fccad8ea091539a16eec9af47c0ed

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Citations in the corpus

Hyperons and massive neutron stars: Vector repulsion and SU(3) symmetry (2011, methodology): “ [15, 16, 17]. In more sophisticated models such as the Brueckner-HartreeFock, the maximum neutron star masses were found to be lower than 1.4M⊙, which is in contradiction with observed pulsar masses [2, 3, 4, 19, 20, 21, 22]. Forourinvestigations, we employ aRelativistic Mean Field(RMF)model, in wh”
The Kerr metric (2014, background): “5M⊙, with an absolute upper bound around 3M⊙ (for a recent review and references, see [151]).”
Unified equation of state for neutron stars on a microscopic basis (2015, background): “It turns out that BHF calculations using realistic hyperon-nucleon interactions known in the literature produce a too soft NS matter EoS and the maximum mass is reduced to values well below the observational limit (Schulze et al. 2006; Schulze & Rijken 2011).”
The Nuclear Symmetry Energy (2016, background): “pressure. The structure of NS could be more complex than described above. In fact exotic matter, like hyperonic or quark matter could appear in the core. A review on this problem can be found in ref. [119]. If this possibility is indeed realized inside NS, then a dierent prospect should be taken, si”
A two-solar-mass neutron star measured using Shapiro delay (2010, unknown): “5051(5) s Declination (J2000) 222u 309 31.”
Strangeness in nuclei and neutron stars (2020, unknown): “[372–378]), or microscopical models (see [292, 307, 309–316, 379] as examples).”