PPT-Symmetry energy in the neutron star equation of state

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. 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.. By: Spencer Weinstein, Mary Yen, Christine Ziegler. Respect The Calculus!. Students Will Be Able To . identify different types of symmetry and. review how to find the x- and y- intercepts of an equation.. 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. . 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. Array for Sub-. F. ermi . E. nergy . H. eavy Ion . R. eaction . D. ynamics. Summer REU Program 2012. Brittany Abromeit. August 3, 2012. 1. Outline:. Supernovae and the resulting neutron stars. Nuclear Equation of State. 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. progenitors a simple mass relationship?. John . Bray. PhD candidate. Supervisor Dr. J.J Eldridge. Crab nebula : . Image Credit : . NASA, ESA, J. Hester, A. Loll (ASU). Outline. The evidence for `kicks’. 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. T. . Sako. Status of the . RHICf. experiment. Cross section. . measurement. （. LHCf. low energy extension. ）. 1. Physics targets of . RHICf. Cross section measurements of very forward particle production for cosmic-ray physics . . 1. Important questions. .  . B. . What observables are sensitive to the EOS and at what densities. ?. 0. Astrophysical observables (neutron stars). . . 1. Binding energies . . 2. Radii of neutron and proton matter in nuclei . EoS. into HI Collisions. Nanxi. . Yao. ICASU, . University of Illinois, Urbana-Champaign. 1. Collaborators: D. . Oliinychenko. , A. Sorensen, V. . Dexheimer. and J. Noronha-Hostler. Using HIC to constrain NS EOS. 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...