PPT-Neutron

Irradiation Measurement for Superconducting Magnet Materials at Low Temperature Tatsushi NAKAMOTO KEK CollaboratorsSupporters KEK M Yoshida M Sugano M Iio S Mihara H . Richard Kouzes. Ken Conlin, James Ely, Luke Erikson, Azaree Lintereur, Emily Mace, Edward Siciliano, Daniel Stephens, David Stromswold, Renee Van Ginhoven, Mitch Woodring. Pacific Northwest National Laboratory. A.. S. . Chepurnov. . a. ,. . V.Y. . Ionidi. . a. , . O.O. . Ivashchuk. . b. , . A.S. . Kubankin. . b. ,. c. , . . A.N. . Oleinik. . b. ,. . A.V. Shchagin . b. ,. d. a . Skobeltsyn. Institute of Nuclear Physics, . Phil Rosenfield, . Fridolin. Weber, Horst . Lenske. Outline. Neutron stars: a short synopsis. The structure of neutron stars. Modeling neutron stars. The equation of state. . Rotating or non-rotating. . Ana Becerril-Reyes, Sanjib S. Gupta and Hendrik Schatz. . Comparison between the two compilations of electron capture rates:. We start by comparing the EC rates at the lowest values of temperature and density (T9=0.01 and Log. By. . Kraml E.. 09.01.2017. A Neutron-Star. (not . actually. ). The Sun. Source: NASA. A Neutron-Star. Comparison. Diameter:. Mass. :. Density. :. Diameter:. Mass. :. Density. :. 1.4 x 10^6 km. 2 x 10^30 kg. Rauno . Julin. Accelerator Laboratory. Department . of Physics . . University of . Jyväskylä. . JYFL. Finland. Nuclear spectrocopy . is required to understand behaviour of nuclei far from stability. D. iffraction at HFIR HB-3A. flipper. Collimator with guide field. S-bender supermirror polarizer. HB-3A. High neutron polarization ratio (>94%) and a good transmission (16% based on the diffraction on a 2 mm size . Farrukh. J. . Fattoyev. My TAMUC collaborators: . B.-A. Li, W. G. Newton . My outside collaborators: . C. J. Horowitz, J. . Piekarewicz. , G. . Shen. , J. . Xu. Texas A&M University-Commerce. International Workshop on Nuclear Dynamics and Thermodynamics.  . On behalf of Sichuan University CDEX Group. Haoyang. Xing. . School of Physical Science and Technology, Sichuan University. Symposium of Sino-German GDT. 2013/4/11. 1. CDEX Collaboration. Outline. 20.11. 1. Neutron stars. T. he . remains of cores of some massive stars that have become supernovae. .. Cores are . a degenerate gas of mostly neutrons.. So much compression at each stage of core contraction that final radius is . R. . . A. . . Akbarov. a,b,c. , . S. . . M. . . Nuruyev. a,b. , . G. . . S. . . Ahmadov. a,b,c. , Z. . . Y. . . Sadiqov. a,c. , . F. . . Ahmadov. b,c. , . S. . Tyutyunnikov. a. , . A. . Sadigov. b,c. V. . Variale*. , B. Skarbo. 2. 1Istituto Nazionale Fisica Nucleare,INFN Sezione di Bari, Italy. 2 . Budcker. Institute of Nuclear Physics, Novosibirsk, Russia. * Vincenzo Variale. Tel.: +39 080 5442344; fax: +39 080 5443190.. Y. . Kanada-En’yo. (Kyoto Univ.). Lesson1: Introduction of cluster phenomena. Lesson2: . Antisymmetrized. molecular dynamics. Lesson3: . clustering in neutron-rich . Be. Norihiro. Matsuda. 1. , Yosuke Iwamoto. 1. , . Tatsuhiko. Sato. 1. , . Shintaro. Hashimoto. 1. , . Tatsuhiko. Ogawa. 1. , Takuya Furuta. 1. , Shinichiro Abe. 1. , Takeshi Kai. 1. , . Ryuji . Hosoyamada.