Hybrid protoneutron stars with the Dyson-Schwinger quark model

Chen, H.; Baldo, M.; Burgio, G. F.; Schulze, H.-J.

doi:10.1103/physrevd.86.045006

Cited by 48 publications

(47 citation statements)

References 87 publications

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“…However, the appearance of hyperons in beta stable matter would strongly decrease the maximum mass of the star [13][14][15][16][17], therefore in this situation presentation of a non baryonic phase like the quark matter could be a feasible way * S.khanmohamadi@ut.ac.ir † hmoshfegh@ut.ac.ir ‡ Atashbart@gmail.com to stiffen the EoS and reaching to massive NS. Thus, a heavy NS can be a hybrid star (HS) [18]. It would have been ideal if there was a unified theory which could have treated both the hadronic and quark phases simultaneously in all ranges of temperatures and densities, but unfortunately, there is no such a reliable theory up to now.…”

Section: Introductionmentioning

confidence: 99%

Hybrid star within the framework of a lowest-order constraint variational method

Khanmohamadi¹,

Moshfegh²,

Tehrani³

2020

Phys. Rev. D

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The hadron-quark phase transition in the core of heavy neutron star has been stuided. For the hadronic sector, we have used the lowest order constraint variational (LOCV) method by employing AV18, AV14, U V14 as well as Reid 68 two-body nucleon-nucleon forces (2BF) supplemented by the phenomenological Urbana-type (UIX) three-body force (TBF). We have adopted the MIT bag model and three-flavor version of Nambu, Jona, Lasinio (NJL) model to describe the quark phase. The Equation of State (EoS) of hybrid star is presented by combining two EoS's of hadronic sector and quark sector of star which are derived from independent models or theories. The hadronquark transition is constructed by considering a sharp phase transition a.k.n. Maxwell construction. The structure of hybrid star is calculated and reported by solving Tolman-Oppenheimer-Volkoff (TOV) equations. Under MIT bag model, stable hybrid star with pure quark phase, as well as hadron-quark mixture in the core is predicted. Where as, under NJL model, hybrid star in the best case scenario, with a mixed but not pure quark phase in the core is predictable. When the AV18 potential supplemented by the TBF is combined with the MIT bag model, the maximum mass of 1.50M⊙(1.945M⊙) would be found for a stable hybrid star with pure quark (mixed phase) core; while the maximum mass of 1.998M⊙ would be calculated under NJL model. A comprehensive analysis on the structure has been conducted for various EoS's of the hadron sector and several parameter sets of the quark EoS's. The results achieved in this study are in strong concurrence with the other calculations reported on this subject.

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Section: Introductionmentioning

confidence: 99%

Hybrid star within the framework of a lowest-order constraint variational method

Khanmohamadi¹,

Moshfegh²,

Tehrani³

2020

Phys. Rev. D

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“…The impact of these additional particles on the evolution of PNSs has a long history; see, e.g., [16] for an early review. Most models employ EoSs for homogeneous matter, neglecting inhomogeneous matter in the outer layers and the formation of a crust; see, e.g., [17][18][19][20][21][22][23][24][25].…”

Section: Introductionmentioning

confidence: 99%

New temperature dependent hyperonic equation of state: Application to rotating neutron star models and I−Q relations

et al. 2017

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In this work we present a newly constructed equation of state (EoS), applicable to stellar core collapse and neutron star mergers including the entire baryon octet. Our EoS is compatible with the main constraints from nuclear physics and, in particular, with a maximum mass for cold β-equilibrated neutron stars of 2M in agreement with recent observations. As an application of our new EoS, we compute numerical stationary models for rapidly (rigidly) rotating hot neutron stars. We consider maximum masses of hot stars, such as protoneutron stars or hypermassive neutron stars in the postmerger phase of binary neutron star coalescence. The universality of I -Q relations at nonzero temperature for fast rotating models, comparing a purely nuclear EoS with its counterparts containing hyperons or the entire baryon octet, respectively, is discussed, too. We find that the I -Q universality is broken in our models when thermal effects become important, independent on the presence of entropy gradients. Thus, the use of I -Q relations for the analysis of protoneutron stars or merger remnant data, including gravitational wave signals from the last stages of binary neutron star mergers, should be regarded with care.

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“…There are big differences between the MIT and DSM regarding the HQ mixed phase that have been pointed out in Chen et al (2011Chen et al ( , 2012: with the MIT model the HQ phase transition starts at fairly low baryon density and a pure quark phase is reached at not too large density, whereas with the DSM the onset of the mixed phase occurs at higher density and the system remains in the mixed phase even at very large density. Furthermore, hyperons are allowed with the MIT model, where they might appear only in small fractions at low density and are replaced by strange QM at higher density (this can be seen in the central panels of Fig.…”

Section: Internal Compositionmentioning

confidence: 99%

“…An eventual HQ phase transition was modeled within an extended MIT bag model (Nicotra et al 2006a;Yasutake et al 2011) or a more sophisticated quark model, the DysonSchwinger model (DSM; Roberts & Williams 1994;Roberts & Schmidt 2000;Alkofer & von Smekal 2001;Roberts et al 2007;Chen et al 2011Chen et al , 2012.…”

Section: Introductionmentioning

confidence: 99%

Structure of the hadron-quark mixed phase in protoneutron stars

Chen

Burgio

Schulze

et al. 2013

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We study the hadron-quark phase transition in the interior of hot protoneutron stars, combining the Brueckner-Hartree-Fock approach for hadronic matter with the MIT bag model or the Dyson-Schwinger model for quark matter. We examine the structure of the mixed phase constructed according to different prescriptions for the phase transition and the resulting consequences for stellar properties. We find important effects for the internal composition, but only very small influence on the global stellar properties.

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Hybrid protoneutron stars with the Dyson-Schwinger quark model

Cited by 48 publications

References 87 publications

Hybrid star within the framework of a lowest-order constraint variational method

Hybrid star within the framework of a lowest-order constraint variational method

New temperature dependent hyperonic equation of state: Application to rotating neutron star models and I−Q relations

Structure of the hadron-quark mixed phase in protoneutron stars

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