Maximum mass of hyperon stars with the Nijmegen ESC08 model

Schulze, H.-J.; Rijken, Th. A.

doi:10.1103/physrevc.84.035801

Cited by 167 publications

(182 citation statements)

References 48 publications

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“…Realistic parameter sets should have a U N below the KaoS constraint up to densities of n ∼ (2 − 3) n 0 . The TM1 [61] parametrization as well as the BruecknerHartree-Fock approximation (BHF) [62][63][64][65] fulfill this requirement. For a RMF model with n 0 = 0.17 fm −3 and K 0 = 220 MeV, we arrive at m * /m = (0.53 − 0.65) for n ∼ (2 − 3) n 0 while for K 0 = 250 MeV we obtain m * /m = (0.54 − 0.67) for the same density range.…”

Section: Maximum Neutron Star Massesmentioning

confidence: 99%

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Sagert

Tolós

Chatterjee³

et al. 2012

Phys. Rev. C

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Measurements of kaon production at subthreshold energies in heavy-ion collisions point to a soft nuclear equation-of-state for densities up to 2-3 times nuclear matter saturation density. We apply these results to study the implications on compact star properties, especially in the context of the recent measurement of the two solar mass pulsar PSR J1614-2230. The implications are twofold: Firstly, the heavy-ion results constrain nuclear matter at densities relevant to light neutron stars. Hence, a radius measurement could provide information about the density dependence of the symmetry energy which is a crucial quantity in nuclear physics. Secondly, the information on the nucleon potential obtained from the analysis of the heavy-ion data can be combined with restrictions from causality on the nuclear equation-of-state. From this we can derive a limit for the highest allowed compact star mass of three solar masses.

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Section: Maximum Neutron Star Massesmentioning

confidence: 99%

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Sagert

Tolós

Chatterjee³

et al. 2012

Phys. Rev. C

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“…Purely nucleonic EOS are able to accommodate masses comparable with this large value [2][3][4][5][6]. However, the appearance of hyperons in beta-stable matter could strongly reduce the maximum mass that can be reached by a baryonic EOS [6][7][8][9][10]. In this case the presence of nonbaryonic, i.e, "quark" matter would be a possible manner to stiffen the EOS and reach large NS masses.…”

Section: Introductionmentioning

confidence: 99%

Hybrid stars with the Dyson-Schwinger quark model

et al. 2011

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We study the hadron-quark phase transition in the interior of neutron stars. For the hadronic sector, we use a microscopic equation of state involving nucleons and hyperons derived within the Brueckner-HartreeFock many-body theory with realistic two-body and three-body forces. For the description of quark matter, we employ the Dyson-Schwinger approach and compare with the MIT bag model. We calculate the structure of neutron star interiors comprising both phases and find that with the Dyson-Schwinger model, the hadron-quark phase transition takes place only when hyperons are excluded, and that a two-solar-mass hybrid star is possible only if the nucleonic equation of state is stiff enough.

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“…Concerning hyperons, simple energetic considerations suggest that they should be present at high density [10]. However, in the standard picture the opening of hyperon degrees of freedom leads to a considerable softening of the equation of state [10][11][12][13][14][15][16][17], which in turns leads to maximum neutron star masses smaller than the highest values obtained in recent observations [18]. This puzzling situation implies that the hyperon-hyperon and hyperon-nucleon couplings must be much more repulsive at high density than presently assumed [19][20][21][22][23][24][25], and/or that something is missing in the present modelization.…”

Section: Introductionmentioning

confidence: 99%

Phase transition toward strange matter

2012

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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.

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Maximum mass of hyperon stars with the Nijmegen ESC08 model

Cited by 167 publications

References 48 publications

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Hybrid stars with the Dyson-Schwinger quark model

Phase transition toward strange matter

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