Quark-hadron crossover equations of state for neutron stars: Constraining the chiral invariant mass in a parity doublet model

Takuya, Minamikawa,; Kojo, Toru; Harada, Masayasu

doi:10.1103/physrevc.103.045205

Cited by 33 publications

(15 citation statements)

References 55 publications

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“…Fig. 2 in [9] and [8,17,19,34,35,39,40,[45][46][47][48][49][50][51][52][61][62][63][64][65][66][67][68][69][70][71][72][73]. Reason (ii) could be related to first-order phase transitions [38,44,52,[74][75][76][77][78] or an "unphase transition", as predicted by the quarkionic model [35,40,42,48,79,80] or crossover transitions/Gibbs constructions to/with (stiff) quark matter [36,37,45,51,[81][82][83]…”

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confidence: 99%

The slope, the hill, the drop, and the swoosh: Learning about the nuclear matter equation of state from the binary Love relations

Tan,

Dexheimer,

Noronha-Hostler

et al. 2021

Preprint

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Analyses that connect astrophysical observations of neutron stars with nuclear matter properties sometimes rely on equation-of-state insensitive relations. We show that the slope of the binary Love relations (i.e. between the tidal deformabilities of binary neutron stars) encodes the rate of change of the nuclear matter speed of sound below three times nuclear saturation density. Twin stars lead to relations that present a signature "hill," "drop," and "swoosh" due to the second (mass-radius) stable branch, requiring a new description of the binary love relations.

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confidence: 99%

The slope, the hill, the drop, and the swoosh: Learning about the nuclear matter equation of state from the binary Love relations

Tan,

Dexheimer,

Noronha-Hostler

et al. 2021

Preprint

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show abstract

“…In QCD, early constructions on NS EoS with the continuity scenario were largely based on interpolations between hadronic and quark EoS [55][56][57][58][59][60][61][62][63][64][65][66]. They found several qualitative trends, such as a peak in the sound velocity, relatively large strangeness fraction at n B 5n 0 , and the importance of semi-short range correlations.…”

Section: Introductionmentioning

confidence: 99%

Peaks of sound velocity in two color dense QCD: quark saturation effects and semishort range correlations

Kojo,

Suenaga

2021

Preprint

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We discuss stiffening of dense matter in two color QCD (QC2D) where hadrons are mesons and diquark baryons. We study two models which describe a transition of matter from the Bose-Einstein-Condensation regime at low density to the Bardeen-Cooper-Schrieffer regime at high density. The first model is based on coherent states of diquarks, and the second is the Nambu-Jona-Lasinio model with diquark pairing terms. We particularly focus on how quark states are occupied as baryon density increases. We find that, due to the occupied quark levels, the ideal gas picture of diquarks breaks down at density significantly less than the density where baryon cores overlap. The saturation of quark states at low momenta stiffens equations of state. We also study the effects of interactions which depend on the quark occupation probability. We argue that equations of state become very stiff when the bulk part of the quark Fermi sea has the effective repulsion but the Fermi surface enjoys the attractive correlations. This disparity for different momentum domains is possible due to the strong channel dependence in gluon exchanges with momentum transfer of 0.2 − 1 GeV. These concepts can be transferred from QC2D to QCD in any numbers of colors.

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“…Such properties of the chiral partners can be described in the framework of the parity doublet model [23][24][25]. The model has been applied to hot and dense hadronic matter, neutron stars (see, e.g, [26][27][28][29][30][31][32][33][34][35][36][37][38]).…”

Section: Introductionmentioning

confidence: 99%

Reconciling multi-messenger constraints with chiral symmetry restoration

Marczenko,

Redlich,

Sasaki

2021

Preprint

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We analyze the recent nuclear and astrophysical constraints in the context of a hadronic equation of state (EoS), in which the baryonic matter is subject to chiral symmetry restoration. We show that it is possible to reconcile the modern constraints on the neutron star (NS) radius and tidal deformability (TD) in the light of recent neutron skin thickness measurement by PREX-II experiment. We find that the softening of the EoS (required by the TD constraint) followed by a subsequent stiffening (required by the 2 M constraint) is driven by the appearance of ∆ matter due to partial restoration of chiral symmetry. Sufficiently early onset of ∆ matter lifts the tension between the results from the PREX-II experiment and TD from GW170817. We argue that a purely hadronic EoS that accounts for the fundamental properties of quantum chromodynamics (QCD) linked to the dynamical emergence of parity doubling with degenerate masses can be fully consistent with the nuclear and astrophysical constraints.

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Quark-hadron crossover equations of state for neutron stars: Constraining the chiral invariant mass in a parity doublet model

Cited by 33 publications

References 55 publications

The slope, the hill, the drop, and the swoosh: Learning about the nuclear matter equation of state from the binary Love relations

The slope, the hill, the drop, and the swoosh: Learning about the nuclear matter equation of state from the binary Love relations

Peaks of sound velocity in two color dense QCD: quark saturation effects and semishort range correlations

Reconciling multi-messenger constraints with chiral symmetry restoration

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