Estimation of the effect of hyperonic three-body forces on the maximum mass of neutron stars

Vidaña, Isaac; Logoteta, Domenico; Providência, C.; Polls, A.; Bombaci, Ignazio

doi:10.1209/0295-5075/94/11002

Cited by 174 publications

(221 citation statements)

References 55 publications

Supporting

Mentioning

210

Contrasting

Order By: Relevance

“…[30,31]) are scarce. This lack of experimental information induces large uncertainties within the microscopic approaches [11][12][13], which suffer in addition probably from theoretical shortcomings, among others due to the unknown hyperonic threebody forces [32]. Phenomenological extrapolations of the low-density behavior within mean field models are subject to large uncertainties, too.…”

Section: Introductionmentioning

confidence: 99%

Phase transition toward strange matter

2012

View full text Add to dashboard Cite

The phase diagram of a system constituted of neutrons and Λ-hyperons in thermal equilibrium is evaluated in the mean-field approximation. It is shown that this simple system exhibits a complex phase diagram with first and second order phase transitions. Due to the generic presence of attractive and repulsive couplings, the existence of phase transitions involving strangeness appears independent of the specific interaction model. In addition we will show under which conditions a phase transition towards strange matter at high density exists, which is expected to persist even within a complete treatment including all the different strange and non-strange baryon states. The impact of this transition on the composition of matter in the inner core of neutron stars is discussed.

show abstract

Section: Introductionmentioning

confidence: 99%

Phase transition toward strange matter

2012

View full text Add to dashboard Cite

show abstract

“…Since then the ΛNN interaction received considerable attention in many other studies of hypernuclei [35][36][37][38][39][40][41][42][43]. It is thus quite natural to expect that YTBIs can influence the EoS of dense matter and can represent a likely candidate to solve the hyperon puzzle [45][46][47][48]. This idea was advocated [49] even before the measurements of NSs with M ∼ 2 M sun [2,3].…”

Section: Hyperon Starsmentioning

confidence: 99%

“…Assuming that the strength of these interactions is either smaller or as large as the pure nucleonic ones, the authors of [45] found that in the most favourable case the relative increase of M max due to YTBIs is ∼ 16% and the largest value of M max for hyperon stars is ∼ 1.6M sun .…”

Section: Hyperon Starsmentioning

confidence: 99%

The Hyperon Puzzle in Neutron Stars

Bombaci

2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

View full text Add to dashboard Cite

The so called hyperon puzzle, i.e. the difficulty to reconcile the measured masses of neutron stars (NSs) with the presence of hyperons in their interiors, is one of the hot topics in astrophysics which is stimulating copious experimental and theoretical research in hypernuclear physics. After illustrating the origin of the hyperon puzzle, I discuss some of its possible solutions, and particularly those related to the role of hyperonic two-and three-body interactions on the equation of state of dense matter. Afterward, I discuss a possibility to circumvent the hyperon puzzle allowing for the presence of strangeness in NSs in the form of deconfined strange quark matter, and thus considering the so called quark stars, i.e. hybrid stars or strange stars. Finally I discuss the astrophysical consequences of the possible conversion process of an hadronic star to a quark star.

show abstract

“…This has to be ascribed to the combination of an incomplete knowledge of the forces governing the system (in the hypernuclear case both two-and three-body ones), and to the concurrent use of approximated theoretical many-body techniques. Some classes of methods extended to the hyperonic sector predict the appearance of hyperons at around 2 − 3ρ 0 , and a strong softening of EOS, implying a sizable reduction of the maximum mass [36][37][38][39]. On the other hand, other approaches suggest much weaker effects arising from the presence of strange baryons in the core of the star [40][41][42][43][44][45].…”

Section: Neutron Matter At High Densitymentioning

confidence: 99%

The EOS of Neutron Matter and the Effect of Λ Hyperons to Neutron Star Structure

Gandolfi

Lonardoni

2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

View full text Add to dashboard Cite

The structure of neutron stars is determined by the equation of state of the matter inside the star, which relies on the knowledge of nuclear interactions. While radii of neutron stars mostly depend on the equation of state of neutron matter at nuclear densities, their maximum mass can be drastically affected by the appearance of hyperons at higher densities in the inner core of the star. We summarize recent quantum Monte Carlo results on the calculation of the equation of state of neutron matter at nuclear and higher densities. We report about the development of realistic hyperon-nucleon interactions based on the available experimental data for light-and medium-heavy hypernuclei and on the effect of Λ hyperons to the neutron star structure.

show abstract

Estimation of the effect of hyperonic three-body forces on the maximum mass of neutron stars

Abstract: PACS 13.75.Ev -Hyperon-nucleon interactions PACS 26.60.Kp -Equations of state of neutron-star matter PACS 26.60.-c -Nuclear matter aspects of neutron stars PACS 97.60.Jd -Neutron stars

Cited by 174 publications

References 55 publications

Phase transition toward strange matter

Phase transition toward strange matter

The Hyperon Puzzle in Neutron Stars

The EOS of Neutron Matter and the Effect of Λ Hyperons to Neutron Star Structure

Contact Info

Product

Resources

About