Hyperons in Neutron Stars

Logoteta, Domenico

doi:10.3390/universe7110408

Cited by 21 publications

(17 citation statements)

References 267 publications

(332 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…They affect the stellar structure and evolution in various ways, see e.g. Burgio et al (2021); Logoteta (2021) for recent reviews. The formation of hyperons inside neutron stars may lead to a significant softening of the EOS of a neutron-star core, with respect to the npeµ case, and lower the theoretical maximum mass below the observed pulsar masses, causing the well-known hyperon puzzle problem (e.g., Burgio et al 2011;Lonardoni et al 2015;Bombaci 2017).…”

Section: Discussionmentioning

confidence: 99%

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Sun¹,

Miao²,

Sun³

et al. 2022

Preprint

View full text Add to dashboard Cite

Hyperons are essential constituents in the neutron star interior. The poorly-known hyperonic interaction is a source of uncertainty for studying laboratory hypernuclei and neutron star observations. In this work, we perform Bayesian inference of phenomenological hyperon-nucleon interactions using the tidal-deformability measurement of the GW170817 binary neutron star merger as detected by LIGO/Virgo and the mass-radius measurements of PSR J0030+0541 and PSR J0740+6620 as detected by NICER. The analysis is based on six relativistic neutron-star-matter equation of states with hyperons from the relativistic mean-field theory, naturally fulfilling the causality requirement and empirical nuclear matter properties. We specifically utilize the strong correlation recently deduced between the scalar and vector meson hyperon couplings, imposed by the measured Λ separation energy in single-Λ hypernuclei, and perform four different tests with or without the strong correlation. We find that the laboratory hypernuclear constraint ensures a large enough Λ-scalar-meson coupling to match the large vector coupling in hyperon star matter. When adopting the current most probable intervals of hyperon couplings from the joint analysis of laboratory and astrophysical data, we find the maximum mass of hyperon stars is at most 2.176 +0.085 −0.202 M (1σ credible interval) from the chosen set of stiff equation of states. The reduction of the stellar radius due to hyperons is quantified based on our analysis and various hyperon star properties are provided.

show abstract

Section: Discussionmentioning

confidence: 99%

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Sun¹,

Miao²,

Sun³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…For instance, the hyperonic NS cores are widely discussed, see, e.g. [154] for a review. Transport coefficients for the hypernuclear NS cores can be in principle, calculated using the similar formalism as studied here.…”

Section: Discussionmentioning

confidence: 99%

Transport coefficients of magnetized neutron star cores

Shternin,

Ofengeim

2022

Preprint

View full text Add to dashboard Cite

We review the calculations of the kinetic coefficients (thermal conductivity, shear viscosity, momentum transfer rates) of the neutron star core matter within the framework of the Landau Fermi-liquid theory. We restrict ourselves to the case of normal (i.e. nonsuperfluid) matter. As an example we consider simplest npeµ composition of neutron star core matter. Utilizing the CompOSE database of dense matter equations of state and several microscopic interactions we analyze the uncertainties in calculations of the kinetic coefficients that result from the insufficient knowledge of the properties of the dense nuclear matter and suggest possible approximate treatment. In our study we also take into account non-quantizing magnetic field. The presence of magnetic field makes transport anisotropic leading to the tensor structure of kinetic coefficients. We find that the moderate (B 10 12 G) magnetic field do not affect considerably thermal conductivity of neutron star core matter, since the latter is mainly governed by the electrically neutral neutrons. In contrast, shear viscosity is affected even by the moderate B ∼ 10 8 − 10 10 G. Based on the in-vacuum nucleon interactions we provide practical expressions for calculation of transport coefficients for any equation of state of dense matter.

show abstract

“…At high densities, hyperonic degrees of freedom may emerge within the cores of neutron stars; for recent reviews on the subject, see Refs. [286][287][288]. These may also participate in BNV interactions, either among themselves or with the nucleons [262], that are, at best, poorly constrained.…”

Section: Effects In Neutron Starsmentioning

confidence: 99%

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Berryman,

Gardner,

Zakeri

2022

Preprint

View full text Add to dashboard Cite

The neutron lifetime anomaly has been used to motivate the introduction of new physics with hidden-sector particles coupled to baryon number, and on which neutron stars provide powerful constraints. Although the neutron lifetime anomaly may eventually prove to be of mundane origin, we use it as motivation for a broader review of the ways that baryon number violation, be it real or apparent, and dark sectors can intertwine and how neutron star observables, both present and future, can constrain them.

show abstract

Hyperons in Neutron Stars

Cited by 21 publications

References 267 publications

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Transport coefficients of magnetized neutron star cores

Neutron Stars with Baryon Number Violation, Probing Dark Sectors

Contact Info

Product

Resources

About