Neutron Stars With Kaon Condensation in Relativistic Effective Model

Wu, Chen; Qian, Wei-Liang; Ma, Yugang; Yang, Jingwei

doi:10.1142/s0218301313500262

Cited by 7 publications

(6 citation statements)

References 43 publications

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“…F lm and G lm denote the antisymmetric tensors of vector fields x and q, respectively [21]. Note that K v is the coupling first introduced in Ref.…”

Section: Effective Masses and Nuclear Mattermentioning

confidence: 99%

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Asymmetric neutron stars in the presence of vacuum fluctuations

Guan

Yang

2016

NUCL SCI TECH

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“…F lm and G lm denote the antisymmetric tensors of vector fields x and q, respectively [21]. Note that K v is the coupling first introduced in Ref.…”

Section: Effective Masses and Nuclear Mattermentioning

confidence: 99%

“…We will also investigate how the properties of neutron matter are affected. Our results will be compared to these obtained in the FSUGold model [20,21].…”

Section: Introductionmentioning

confidence: 98%

Asymmetric neutron stars in the presence of vacuum fluctuations

Guan

Yang

2016

NUCL SCI TECH

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“…After the detection of the Gravitational Wave, i.e., the GW170817 of Binary Neutron Star (BNS) merging event [5], the tidal deformability provides an extra constraint on the EOS, Λ < 800 for the 1.4-solar-mass compact stars, which rules out many stiff EOS with large tidal deformabilities. Considering these strict constraints, it is commonly believed that neutron stars encompass "normal" stars [6][7][8][9][10] and "strange quark matter" stars [11]. The concept of strange quark matter stars originated from Witten's strange quark matter hypothesis.…”

Section: Introductionmentioning

confidence: 99%

The chiral restored quark stars can exist in the universe

Su,

Yan,

et al. 2021

Preprint

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In this paper, the equation of state (EOS) of deconfined quark stars is studied in the framework of the twoflavor NJL model, and the self-consistent mean field approximation is employed by introducing a parameter α combining the original Lagrangian and the Fierz-transformed Lagrangian, L R = (1 − α)L + αL F , to measure the weights of different interaction channels. It is believed that the deconfinement of phase transition happens along with the chiral phase transition. Thus, due to the lack of description of confinement in the NJL model, the vacuum pressure is set to confine quarks at low densities, which is the pressure corresponding to the critical point of chiral phase transition. We find that deconfined quark stars can reach over two-solar-mass, and the bag constant therefore shifts from (130 MeV) 4 to (150 MeV) 4 as α grows. In addition, the tidal deformability Λ is yielded ranging from 253 to 482 along with the decrease of α, which satisfies the astronomical constraint of Λ < 800 for 1.4-solar-mass neutron stars.

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“…In 1986, Kaplan and Nelson pointed out that K − mesons can form the Bose-Einstein condensed phases in dense nuclear matter [20]. Antikaon condensed phases can soften the EOSs, change the whole properties of NSs [21][22][23][24][25][26][27][28][29][30], and significantly improve the protonic 1 S 0 superfluids in a NS core [31]. We now investigate how a NS cooling rate changes if the protonic 1 S 0 superfluids appear in the massive NS with antikaon condensed phases.…”

Section: Introductionmentioning

confidence: 99%

Nucleonic Direct Urca Processes and Cooling of the Massive Neutron Star by Antikaon Condensations

Ding

Liu

et al. 2020

Advances in Astronomy

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Nucleonic direct Urca processes and cooling of the massive neutron stars are studied by considering antikaon condensations. Calculations are performed in the relativistic mean field and isothermal interior approximations. Neutrino energy losses of the nucleonic direct Urca processes are reduced when the optical potential of antikaons changes from − 80 to − 130 MeV. If the center density of the massive neutron stars is a constant, the masses taper off with the optical potential of antikaons, and neutrino luminosities of the nucleonic direct Urca processes decrease for ρ CN = 0.5 fm − 3 but first increase and then decrease for larger ρ CN . Large optical potential of antikaons results in warming of the nonsuperfluid massive neutron stars. Massive neutron stars turn warmer with the protonic S 0 1 superfluids. However, the decline of the critical temperatures of the protonic S 0 1 superfluids for the large optical potential of antikaons can speed up the cooling of the massive neutron stars.

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Neutron Stars With Kaon Condensation in Relativistic Effective Model

Cited by 7 publications

References 43 publications

Asymmetric neutron stars in the presence of vacuum fluctuations

Asymmetric neutron stars in the presence of vacuum fluctuations

The chiral restored quark stars can exist in the universe

Nucleonic Direct Urca Processes and Cooling of the Massive Neutron Star by Antikaon Condensations

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