Hyperons in neutron star matter within relativistic mean-field models

By M. Oertel, Constança Providência, F. Gulminelli, Adriana Raduta. Physics of particles and nuclei, 2014

133 citations recorded by the source corpus.

Since the discovery of neutron stars with masses around 2M⊙ the composition of matter in the central part of these massive stars has been intensively discussed. Within this paper we will (re)investigate the question of the appearance of hyperons. To that end we will perform parameter study within relativistic mean field models. We will show that it is possible to obtain high mass neutron stars with a substantial amount of hyperons and a spinodal instability at the onset of hyperons. The results depend strongly on the interaction in the hyperon-hyperon channels, on which only very little information is available from terrestrial experiments up to now.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/28ec1720f19127d4605665debb995ae8749c75ca

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

In Geophysics

Citations in the corpus

Unified equation of state for neutron stars on a microscopic basis (2015, background): “Although relativistic mean field models can be adjusted to accomodate NS masses larger than two solar masses (Oertel et al. 2015), and additional terms in the hyperon-nucleon interaction can provide a possible solution (Yamamoto et al. 2014), this “hyperon puzzle” has to be considered still open…”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “These models only consider nucleons, while other constituents such as hyperons, pions/kaons, or condensates, which may play a role at very high densities, are incorporated in other EOS: the GM1 model [184] based on relativistic mean field calculations (M⋆ ∼ 2.0 − 2.4M⊙), and its extension GM1nph [20”