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reaction rate through direct nuclear reaction theories福井 徳朗; 緒方 一介*; 蓑茂 工将*; 八尋 正信*
JPS Conference Proceedings (Internet), 14, p.020513_1 - 020513_3, 2017/02
被引用回数：0 パーセンタイル：0.00(Astronomy & Astrophysics)The reaction is expected to ignite the hot pp chain and its astrophysical factor at zero energy 
(0) has been evaluated through alternative measurements. However the analyses in their work were done with primitive reaction model, in which the excitation of nuclei in the intermediate state was not properly taken into account. We have reanalyzed the elastic breakup reaction 
and the proton removal reactions 
and 
by means of the method of the continuum-discretized coupled-channels (CDCC). The CDCC is able to calculate distorted waves employing the coupled-channels approach regarding bound-continuum states couplings as well as continuum-continuum ones. Furthermore, in order to analyze the transfer reaction 
, we have constructed the coupled-channels Born approximation (CCBA) model, in which excitation of 
and 
is explicitly taken into account by CDCC.
武藤 巧*; 丸山 敏毅; 巽 敏隆*
JPS Conference Proceedings (Internet), 14, p.020809_1 - 020809_3, 2017/02
被引用回数：0 パーセンタイル：0.00(Astronomy & Astrophysics)Kaon condensation in hyperon-mixed matter, which may be realized in neutron stars, is investigated on the basis of the relativistic mean-field theory for baryon-baryon interaction, combined with the effective chiral Lagrangian. We introduce the range terms for both nucleons and hyperons and a pole contribution from the 
(1405) so as to reproduce the 
-wave on-shell 
scattering lengths. Onset density of kaon condensation in the hyperon-mixed matter and the equation of state (EOS) is obtained. It is shown that coexistence of kaon condensation and hyperon-mixed matter necessarily leads to significant softening of the EOS. We address stiffening effects to make the EOS consistent with recent observations of massive neutron stars.
野田 常雄*; 橋本 正章*; 松尾 康秀*; 安武 伸俊*; 丸山 敏毅; 巽 敏隆*
JPS Conference Proceedings (Internet), 14, p.020805_1 - 020805_3, 2017/02
被引用回数：0 パーセンタイル：0.00(Astronomy & Astrophysics)A neutron star is a highly dense object which lasts after a supernova explosion. The density of a neutron star overcomes the nuclear density, and the temperature is high at the beginning of its history. An isolated neutron star does not have any heat sources, and it cools down emitting thermal energy by neutrinos. The neutrino emission process depends on the state of interior matter of the neutron star. To compare theoretical simulations and observations of neutron stars, it can constrain the nuclear theory of high density region. We create a model of neutron stars with colour superconducting quark matter and nucleon super fluidity / superconductivity, to satisfy recent observations, including two 2
neutron stars. We parameterize these super-states and demonstrate the cooling curves, which show heavy stars do not always cool faster than lighter stars.
Lee, T.-G.*; 西山 和也*; 安武 伸俊*; 丸山 敏毅; 巽 敏隆*
JPS Conference Proceedings (Internet), 14, p.020808_1 - 020808_3, 2017/02
被引用回数：0 パーセンタイル：0.00(Astronomy & Astrophysics)We explore the multi-dimensional structure of inhomogeneous chiral condensates in quark matter. For a one-dimensional structure, the system becomes unstable at finite temperature due to the Nambu-Goldstone excitations. However, inhomogeneous chiral condensates with multi-dimensional modulations may be realized as a true long-range order at any temperature, as inferred from the Landau Peierls theorem. We here present some possible strategies for searching the multi-dimensional structure of chiral crystals.
C(
,
)
O reaction at E
= 1.2 and 1.5 MeV using pulsed beam牧井 宏之; 上田 仁*; 永井 泰樹*; 瀬川 麻里子; 天満 康之*; 嶋 達志*; 三島 賢二*; 井頭 政之*
no journal, ,
C(,)O反応は恒星内He燃焼期における元素合成やその後の恒星進化を理解する上で非常に重要な反応である。しかしながら、これまで様々なグループが報告している断面積の測定結果には大きな不確定性がある。我々は高効率のNaI(Tl)スペクトロメータ, パルスビーム, 標的厚モニターから構成される新しいシステムの構築を行った。この測定システムを用いることでC(,)O反応によって発生した線の角度分布の測定を行い、重心系エネルギー1.2MeV及び、1.5MeVでE1・E2断面積の導出に成功したので、この結果を報告する。
