Spin change of a proto-neutron star by the emission of neutrinos

被引：13

作者：

Ryu, Chung-Yeol ^{[2
]}

Maruyama, Tomoyuki ^{[1
,3
]}

Kajino, Toshitaka ^{[1
,4
]}

Mathews, Grant J. ^{[5
]}

Cheoun, Myung-Ki ^{[1
,6
]}

机构：

[1] Natl Astron Observ, Mitaka, Tokyo 1818589, Japan

[2] Hanyang Univ, Gen Educ Curriculum Ctr, Seoul 133791, South Korea

[3] Nihon Univ, Coll Bioresource Sci, Fujisawa, Kanagawa 2528510, Japan

[4] Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan

[5] Univ Notre Dame, Dept Phys, Ctr Astrophys, Notre Dame, IN 46556 USA

[6] Soongsil Univ, Dept Phys, Seoul 156743, South Korea

来源：

PHYSICAL REVIEW C | 2012年 / 85卷 / 04期

基金：

新加坡国家研究基金会;

关键词：

EVOLUTION; BIRTH;

D O I：

10.1103/PhysRevC.85.045803

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

We investigate the structure of proto-neutron stars (PNSs) with trapped neutrinos by using a quark-meson coupling model. We adopt a phenomenological lepton density which is diffuse near the surface. We calculate the populations of baryons and leptons, the equations of state, and the mass-radius relation for isentropic PNS models. In addition, the moment of inertia is calculated for both PNS and cold-neutron-star (CNS) models as a means to study the change of the spin period due to the neutrino emission from a PNS. Neutrino emission from a hyperonic neutron star is shown to increase the spin by about 10% of the initial spin, while the spin of a nucleonic neutron star with a central density above rho(C) approximate to 5 rho(0) is decreased by a few % by the emission of neutrinos. Therefore, the spin change owing to the leakage of neutrinos from a PNS is a small (<10%) correction compared to other processes related to the spin change.

引用

页数：7

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