PPT-Electron Capture Rates for Neutron Star Crusts.

Ana BecerrilReyes 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 T9001 and Log. Varun Bhalerao. California Institute of Technology. Collaborators: F. Harrison, S. . Kulkarni. , Marten van . Kerkwijk. , and others. Weighing in on Neutron Stars. Varun Bhalerao. Why?. How?. What?. Classes of objects. the Supernova Engine. Bounce Masses. Mass at Explosion. Fallback . Neutron Star Masses. Observations of neutron star binaries provide a growing list of neutron star mass estimates.. Current observations predict a range of NS masses from 1.0 to >2 solar masses.. (Saga Univ.). Dark matter . capture in . c. ompact stars. -stellar constraints on dark matter-. Oct. 20, 2014 . ＠. QCS2014, . KIAA, . Beijin. . Dark matter . capture . . in . Stars: . Insights . into their Formation. , Evolution & . Structure from their. Masses and Radii. Feryal Ozel. University of Arizona. In collaboration with T. . Guver. , M. . Baubock. , L. . Camarota. V. V. . Sargsyan. *. , . G. G. . Adamian. , N. V. . Antonenko. In collaboration with . W. . . Scheid. , H. Q. . Zhang, D. . Lacroix. , G. Scamps. ECT*, Trento, . Italy. *Joint Institute For Nuclear Research. 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. and (. d,p. ) reactions on . Non-Spherical Nuclei. Goran Arbanas . (. ORNL). Ian J. Thompson (LLNL). with. Filomena. . Nunes. (MSU). Jutta. Escher (LLNL). Charlotte . Elster. (OU). TORUS Collaboration. ＠. Baryons2013, Glasgow . Motoi Tachibana (Saga Univ.). Dark matter . capture . in . n. eutron . stars . with exotic . phases. A modern physics perspective. . “. UROBOROS” = unity of matters & universe. . Beta decay. seen at quark level. . . A quark emits a W or W- and changes its flavor (type).. . Beta decay. leading a positron. It travels a short distance before encountering an electron in the material, where it annihilates to two gamma rays (photons) of .511 MeV each.. Prof Wladimir . Lyra. Live Oak, 1119-G. Office Hours: Mon 4pm-5pm. Class hours: Mon/Wed 5pm-6:15pm. Evolution of high mass stars. The evolution we covered in last class is for low mass stars (. M < 4 M. and . astrophysical . observations. David E. . Á. lvarez. . C. .. Sept 2013. S. . Kubis. , D. . Blaschke. and T. . Klaehn. The Modern Physics of Compact Stars and Relativistic Gravity. Outline. Introduction to neutron stars. away. messages:. Elements. . heavier. . than. Fe are . produced. by neutron capture . processes. There . exists. . two. major . categories. of . processes. . with. . low. and . high. . densities. Frederick Seward. ABSTRACT. Neutron stars are predicted to be stable over the mass range ≈ 0.1 to ≈ 3M. ⊙. . At 1.4 M. ⊙. , 98% of the mass is in a core with . supernuclear. density and 1-2 % forms a thin crust and atmosphere . As mass decreases, the fraction of mass in the crust increases until at . Frederick Seward. ABSTRACT. Neutron stars are predicted to be stable over the mass range ≈ 0.1 to ≈ 3M. ⊙. . At 1.4 M. ⊙. , 98% of the mass is in a core with . supernuclear. density and 1-2 % forms a thin crust and atmosphere . As mass...