Strangeness condensation and cooling of neutron stars

Brown, G. E.; Kubodera, K.; Page, Dany; Pizzochero, Pierre M.

doi:10.1103/physrevd.37.2042

Cited by 127 publications

(125 citation statements)

References 19 publications

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“…Its formal calculation is even simpler than for the pion condensed matter because of the stationarity and uniformity of the kaon field. For θ K < ∼ 1, Brown et al (1988) find…”

Section: (A) Pion Condensed Mattermentioning

confidence: 99%

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Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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“…Its formal calculation is even simpler than for the pion condensed matter because of the stationarity and uniformity of the kaon field. For θ K < ∼ 1, Brown et al (1988) find…”

Section: (A) Pion Condensed Mattermentioning

confidence: 99%

“…(4) Following Kaplan and Nelson (1986), Nelson and Kaplan (1987) and Brown et al (1988), several authors considered the hypothesis of kaon condensation. Similarly to pion condensates, kaon condensates may also enhance the neutrino luminosity by several orders of magnitude (Sect.…”

Section: Structure Of Neutron Starsmentioning

confidence: 99%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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“…Various scenarios have been proposed that can lead to a soft EOS. Brown and collaborators suggested that kaon condensation might happen at a critical density of 2-4ρ 0 [28]. The existence of many K − mesons implies the coexistence of a large number of protons that are needed to neutralize the negative charge of K − mesons [29].…”

Section: Introductionmentioning

confidence: 99%

Kaons in dense matter, kaon production in heavy-ion collisions, and kaon condensation in neutron stars

1997

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The recent past witnesses the growing interdependence between the physics of hadrons, the physics of relativistic heavy-ion collisions, and the physics of compact objects in astrophysics. A notable example is the kaon which plays special roles in all the three fields. In this paper, we first review the various theoretical investigations of kaon properties in nuclear medium, focusing on possible uncertainties in each model. We then present a detailed transport model study of kaon production in heavy-ion collisions at SIS energies. We shall discuss especially the elementary kaon and antikaon production cross sections in hadron-hadron interactions, that represent one of the most serious uncertainties in the transport model study of particle production in heavy-ion collisions. The main purpose of such a study is to constrain kaon in-medium properties from the heavy-ion data. This can provide useful guidances for the development of theoretical models of the kaon in medium. In the last part of the paper, we apply the kaon in-medium properties extracted from heavy-ion data to the study of neutron star properties. Based on a conventional equation of state of nuclear matter that can be considered as one of the best constrained by available experimental data on finite nuclei, we find that the maximum mass of neutron stars is about 2M⊙, which is reduced to about 1.5M⊙ once kaon condensation as constrained by heavy-ion data is introduced.pacs: 25.75. Dw, 97.60.Jd, 26.60.+c, 24.10.Lx

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“…Specifically, since the possible existence of antikaon condensation was suggested in neutron stars [1], its implications for astrophysical phenomena have been widely discussed [2,3,4,5]. The examples are effects of softening of the equation of state on the static and dynamic properties of neutron stars [6,7,8,9,10,11,12] and thermal evolution of neutron stars through extra mechanisms of neutrino emission [13,14,15,16,17].…”

Section: Introductionmentioning

confidence: 99%

Kaon condensation and lambda–nucleon loop in the relativistic mean-field approach

et al. 2005

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The possibility of kaon condensation in high-density symmetric nuclear matter is investigated including both s-and p-wave kaon-baryon interactions within the relativistic meanfield (RMF) theory. Above a certain density, we have a collectiveK s state carrying the same quantum numbers as the antikaon. The appearance of theK s state is caused by the time component of the axial-vector interaction between kaons and baryons. It is shown that the system becomes unstable with respect to condensation of K-K s pairs. We consider how the effective baryon masses affect the kaon self-energy coming from the time component of the axial-vector interaction. Also, the role of the spatial component of the axial-vector interaction on the possible existence of the collective kaonic states is discussed in connection with Λ-mixing effects in the ground state of high-density matter. Implications of KK s condensation for high-energy heavy-ion collisions are briefly mentioned.

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Strangeness condensation and cooling of neutron stars

Cited by 127 publications

References 19 publications

Neutrino emission from neutron stars

Neutrino emission from neutron stars

Kaons in dense matter, kaon production in heavy-ion collisions, and kaon condensation in neutron stars

Kaon condensation and lambda–nucleon loop in the relativistic mean-field approach

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