Interaction cross sections for Ne isotopes towards the island of inversion and halo structures of 29Ne and 31Ne
Interaction cross sections for Ne isotopes towards the island of inversion and halo structures of 29Ne and 31Ne
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DOI：
10.1016/j.physletb.2011.12.028
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发表时间：
2012-02
影响因子：
4.4
通讯作者：
M. Takechi;T. Ohtsubo;M. Fukuda;D. Nishimura;T. Kuboki;Takeshi Suzuki;Takayuki Yamaguchi;A. Ozawa;T. Moriguchi;H. Ooishi;D. Nagae;H. Suzuki;S. Suzuki;T. Izumikawa;T. Sumikama;M. Ishihara;H. Geissel;N. Aoi;Rui-jiu Chen;D. Fang;N. Fukuda;I. Hachiuma;N. Inabe;Y. Ishibashi;Y. Ito;D. Kameda;T. Kubo;K. Kusaka;M. Lantz;Yugang Ma;K. Matsuta;M. Mihara;Y. Miyashita;S. Momota;K. Namihira;M. Nagashima;Y. Ohkuma;T. Ohnishi;M. Ohtake;K. Ogawa;H. Sakurai;Y. Shimbara;T. Suda;H. Takeda;S. Takeuchi;K. Tanaka;R. Watanabe;M. Winkler;Y. Yanagisawa;Y. Yasuda;K. Yoshinaga;A. Yoshida;K. Yoshida
中科院分区：
文献类型：
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作者：
M. Takechi;T. Ohtsubo;M. Fukuda;D. Nishimura;T. Kuboki;Takeshi Suzuki;Takayuki Yamaguchi;A. Ozawa;T. Moriguchi;H. Ooishi;D. Nagae;H. Suzuki;S. Suzuki;T. Izumikawa;T. Sumikama;M. Ishihara;H. Geissel;N. Aoi;Rui-jiu Chen;D. Fang;N. Fukuda;I. Hachiuma;N. Inabe;Y. Ishibashi;Y. Ito;D. Kameda;T. Kubo;K. Kusaka;M. Lantz;Yugang Ma;K. Matsuta;M. Mihara;Y. Miyashita;S. Momota;K. Namihira;M. Nagashima;Y. Ohkuma;T. Ohnishi;M. Ohtake;K. Ogawa;H. Sakurai;Y. Shimbara;T. Suda;H. Takeda;S. Takeuchi;K. Tanaka;R. Watanabe;M. Winkler;Y. Yanagisawa;Y. Yasuda;K. Yoshinaga;A. Yoshida;K. Yoshida
在RIBF，RIKEN的BigRIPS装置上，在240 MeV/核子附近测量了Ne同位素从稳定线到中子滴线附近的相互作用截面(σ)。对于稳定核，27-32Ne的σI在任何情况下都超过了σI的系统质量数依赖关系，这可以用考虑核变形来解释。特别是，29Ne和31Ne的σI值显着大于其邻近核素的I值。在假设29Ne(31Ne)价中子占据0d3/2(0f7/2)轨道的假设下，29Ne和31Ne的σI对29Ne和31Ne的这些增强不能用单粒子模型计算来解释。目前的数据表明，29Ne以S为主的晕结构，31Ne以S或p轨道晕为主。
Interaction cross sections (σI) for Ne isotopes from the stability line to the vicinity of the neutron drip line have been measured at around 240 MeV/nucleon using BigRIPS at RIBF, RIKEN. The σIfor27–32Ne in every case exceed the systematic mass-number dependence of σIfor stable nuclei, which can be explained by considering the nuclear deformation. In particular the σIfor29Ne and31Ne are significantly greater than those of their neighboring nuclides. These enhancements of σIfor29Ne and31Ne cannot be explained by a single-particle model calculation under the assumption that the valence neutron of29Ne (31Ne) occupies the 0d3/2(0f7/2) orbital, as expected from the standard spherical shell ordering. The present data suggest an s dominant halo structure of29Ne and s- or p-orbital halo in31Ne.