Melting of antikaon condensate in protoneutron stars

Banik, Sarmistha; Nandi, Rana; Bandyopadhyay, Debades

doi:10.1103/physrevc.86.045803

Cited by 5 publications

(3 citation statements)

References 41 publications

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“…The temperature helps the appearance of kaons (strangeness): they appear at a smaller density as compared will the results presented in [19] for a zero temperature system. Similar results were obtained previously [25,31]. Moreover, it is clear that a larger slope enhances the production of kaons.…”

Section: Resultssupporting

confidence: 90%

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

2014

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In this work we investigate protoneutron star properties within a modified version of the quark-meson coupling (QMC) model that incorporates an ω-ρ interaction plus kaon condensed matter at finite temperature. Fixed entropy and trapped neutrinos are taken into account. Our results are compared with the ones obtained with the GM1 parametrization of the nonlinear Walecka model for similar values of the symmetry energy slope. Contrary to GM1, within the QMC model the formation of low mass black holes during cooling are not probable. It is shown that the evolution of the protoneutron star may include the melting of the kaon condensate driven by the neutrino diffusion, followed by the formation of a second condensate after cooling. The signature of this complex process could be a neutrino signal followed by a gamma ray burst. We have seen that both models can, in general, describe very massive stars.

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Section: Resultssupporting

confidence: 90%

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

2014

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“…Neutron stars were studied within RMF models with the inclusion of hyperons [5][6][7][8][9][10][11][12][13][14][15][16][17][18][19], the antikaon K − [20][21][22][23][24][25][26][27], the antikaons K − andK 0 [28][29][30][31], and both hyperons and antikaons [32][33][34][35][36]. Recently, we have studied the role of antikaons [23,37] in the presence of higher order couplings of the extended RMF models.…”

Section: Introductionmentioning

confidence: 99%

Impact of hyperons and antikaons in an extended relativistic mean-field description of neutron stars

Gupta¹,

Arumugam²

2013

Phys. Rev. C

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We study the role of higher order couplings in extended relativistic mean-field models, along with the condensation of antikaons and hyperons, on neutron star properties. Though this approach seems to be better and inclusive, the results are sensitive to the hyperon-nucleon and antikaon-nucleon coupling constants, which are poorly known. Despite this aspect, we find that both the hyperons and the antikaons can play a significant role, even in extended relativistic mean-field models which yield softer equations of state. We find that there is a strong interplay between antikaons and hyperons affecting each other's influence on neutron star properties. We discuss the implications of our results in light of the recently observed pulsar with 1.97 ± 0.04 solar masses.

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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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Melting of antikaon condensate in protoneutron stars

Cited by 5 publications

References 41 publications

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

Effects of the symmetry energy on the kaon condensates in the quark-meson coupling model

Impact of hyperons and antikaons in an extended relativistic mean-field description of neutron stars

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

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