Relativistic mean-field treatment of pulsar kicks from neutrino propagation in magnetized proto-neutron stars

Maruyama, Tomoyuki; Yasutake, Nobutoshi; Cheoun, Myung-Ki; Hidaka, Jun; Kajino, Toshitaka; Mathews, Grant J.; Ryu, C. Y.

doi:10.1103/physrevd.86.123003

Cited by 21 publications

(30 citation statements)

References 78 publications

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“…After passing by the uniform density region, ρ uni ∼ 6.85 × 10 −2 fm −3 = 1.14 × 10 14 g/cm 3 ∼ 0.5ρ o , which density dissolves a crust of the PNS into the core comprising a uniform plasma of nucleons and leptons, neutrinos enter into the crust * cheoun@ssu.ac.kr † kiseokchoi@gmail.com ‡ kyungsik@kau.ac.kr § koichi.saito@rs.tus.ac.jp kajino@nao.ac.jp ¶ kazuo.tsushima@gmail.com ** maruyama.tomoyuki@nihon-u.ac.jp region of the PNS. This crust region is usually treated as two different parts, inner and outer crusts divided by the neutron drip density, ρ drip ∼ 2.70 × 10 −4 fm −3 = 4.48 × 10 11 g/cm 3 .…”

Section: Introductionmentioning

confidence: 99%

“…This crust region is usually treated as two different parts, inner and outer crusts divided by the neutron drip density, ρ drip ∼ 2.70 × 10 −4 fm −3 = 4.48 × 10 11 g/cm 3 . Beyond this density, neutrons drip out of finite nuclei presumed to be embedded as lattice structures in the outer crust of the neutron star.…”

Section: Introductionmentioning

confidence: 99%

“…For instance, the pulsar kick [2,3] and the spin deceleration [4] of the strongly magnetized neutron stars were shown to be closely associated with the asymmetry, according to detailed studies of the neutrino transport in dense matter by a relativistic mean field theory (RMF).…”

Section: Introductionmentioning

confidence: 99%

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Effects of the density-dependent weak form factors on the neutrino reaction via neutral current for the nucleon in nuclear matter and12C

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Effects of the density-dependent weak form factors on the neutrino reaction via neutral current for the nucleon in nuclear matter and ¹²C Physical Review C, 2013; 87(6) 3. The right to use all or part of the Article, including the APS-prepared version without revision or modification, on the author(s)' web home page or employer's website and to make copies of all or part of the Article, including the APS-prepared version without revision or modification, for the author(s)' and/or the employer's use for educational or research purposes.": February 2014PHYSICAL REVIEW C 87, 065502 (2013) Effects of the density-dependent weak form factors on the neutrino reaction via neutral current for the nucleon in nuclear matter and 12 C The nucleon form factors in free space are usually thought to be modified when a nucleon is bound in a nucleus or immersed in a nuclear medium. We investigate effects of the density-dependent axial and weak-vector form factors on the electroneutrino (ν e ) and anti-electroneutrino (ν e ) reactions with incident energy E ν 80 MeV via neutral current (NC) for a nucleon in a nuclear medium or 12 C. For the density-dependent form factors, we exploit the quark-meson-coupling (QMC) model, and apply them to the ν e andν e induced reactions by NC. About 12% decrease of the total cross section by the ν e reaction on the nucleon is obtained at normal density, ρ = ρ 0 ∼ 0.15 fm −3 , as well as about 18% reduction of the total ν e cross section on 12 C, by the modification of the weak form factors of the bound nucleon. However, similarly to the charged current reaction, effects of the nucleon property change in theν e reaction reduce significantly the cross sections about 30% for the nucleon in matter and 12 C cases. Such a large asymmetry in theν e cross sections is addressed to originate from the different helicities ofν e and ν e .

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Effects of the density-dependent weak form factors on the neutrino reaction via neutral current for the nucleon in nuclear matter and12C

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“…In our previous work [12,15], we calculated neutrino scattering and absorption cross sections in hot, dense magnetized neutron-star matter including hyperons in a relativistic mean field (RMF) theory [16]. We evaluated both the associated pulsar kick velocities [15] and the spin deceleration [17] for PNSs.…”

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confidence: 99%

“…We evaluated both the associated pulsar kick velocities [15] and the spin deceleration [17] for PNSs. When the neutrino momentum is anti-parallel to the magnetic field, the opposite effect occurs in the opposite direction.…”

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confidence: 99%

Asymmetric neutrino production in strongly magnetized proto-neutron stars

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We calculate the neutrino production cross-section in proto-neutron star matter in the presence of a strong magnetic field. We assume isoentropic conditions and introduce a new equation of state parameter-set in the relativistic mean-field approach that can reproduce neutron stars with M > 1.96 M ⊙ as required by observations. We find that the production process increases the flux of emitted neutrinos along the direction parallel to the magnetic field and decreases the flux in the opposite direction. This means that the neutrino flux asymmetry due to the neutrino absorption and scattering processes in a magnetic field becomes larger by the inclusion of the neutrino production process.

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Asymmetry in the neutrino and anti-neutrino reactions in a nuclear medium

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We study the effect of the density-dependent axial and vector form factors on the electro-neutrino (ν e ) and anti-neutrino (ν e ) reactions for a nucleon in nuclear matter or in 12 C. The nucleon form factors in free space are presumed to be modified for a bound nucleon in a nuclear medium. We adopt the density-dependent form factors calculated by the quark-meson coupling (QMC) model, and apply them to the ν e andν e induced reactions with the initial energy E = 8 ∼ 80 MeV. We find that the total ν e cross sections on 12 C as well as a nucleon in nuclear matter are reduced by about 5 % at the nuclear saturation density, ρ 0 . This reduction is caused by the modification of the nucleon structure in matter. Although the density effect for both cases is relatively small, it is comparable with the effect of Coulomb distortion on the outgoing lepton in the ν-reaction. In contrast, the density effect on theν e reaction reduces the cross section significantly in both nuclear matter and 12 C cases, and the amount maximally becomes of about 35 % around ρ 0 . Such large asymmetry in the ν e andν e cross sections, which seems to be nearly independent of the target, is originated from the difference in the helicities ofν e and ν e . It is expected that the asymmetry influences the r-process and also the neutrino-process nucleosynthesis in core-collapse supernovae.

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Relativistic mean-field treatment of pulsar kicks from neutrino propagation in magnetized proto-neutron stars

Cited by 21 publications

References 78 publications

Effects of the density-dependent weak form factors on the neutrino reaction via neutral current for the nucleon in nuclear matter and12C

Effects of the density-dependent weak form factors on the neutrino reaction via neutral current for the nucleon in nuclear matter and12C

Asymmetric neutrino production in strongly magnetized proto-neutron stars

Asymmetry in the neutrino and anti-neutrino reactions in a nuclear medium

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