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Prog. Theor. Phys. Vol. 112 No. 1 (2004) pp. 37-72

[ Full Text PDF : FREE ACCESS (521K) ]

Baryon Superfluidity and Neutrino Emissivity of Neutron Stars

Tatsuyuki Takatsuka1,* and Ryozo Tamagaki2,**

1Faculty of Humanities and Social Sciences,
Iwate University, Morioka 020-0066, Japan
2Kamitakano Maeda-Cho 26-5, Kyoto 606-0097, Japan

(Received April 23, 2004)

Abstract:

For neutron stars with hyperon-mixed cores, neutrino emissivity is studied using the properties of neutron star matter determined under the equation of state, which is obtained by introducing a repulsive three-body force universal for all the baryons so as to assure the maximum mass of neutron stars compatible with observations. The case without a meson condensate is treated. We choose the inputs provided by nuclear physics, with a reliable allowance. Paying attention to the density dependence of the critical temperatures of the baryon superfluids, which reflect the nature of the baryon-baryon interaction and control neutron star cooling, we show what neutrino emission processes are efficient in regions both with and without hyperon mixing. By comparing the calculated emissivities with respect to densities, we can conclude that at densities lower than about 4 times the nuclear density, the Cooper-pair process arising from the neutron 3 P2 superfluid dominates, while at higher densities the hyperon direct Urca process dominates. For the hyperon direct Urca process to be a candidate responsible for rapid cooling compatible with observations, a moderately large energy gap of the Λ-particle 1 S0 superfliud is required to suppress its large emissivity. The implications of these results are discussed in the relation to thermal evolution of neutron stars.


URL : http://ptp.ipap.jp/link?PTP/112/37/
DOI : 10.1143/PTP.112.37


*E-mail: takatuka@iwate-u.ac.jp
**E-mail: tamagaki@yukawa.kyoto-u.ac.jp

[ Full Text PDF : FREE ACCESS (521K) ] Citation:

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