PPT-Constraining Nuclear Symmetry Energy from Converting Neutron Star

EoS into HI Collisions Nanxi Yao ICASU University of Illinois UrbanaChampaign 1 Collaborators D Oliinychenko A Sorensen V Dexheimer and J NoronhaHostler Using HIC to constrain NS EOS. 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. Juan Maldacena. Institute for Advanced Study. . Based on: 1112.1016 and 1204.3882 by J. M. and A. . Zhiboedov. . . Strings 2012. Munich. Elementary particles can have spin. . Even massless particles can have spin. . 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.. isospin. ratio from nucleons to fragments. Yingxun. Zhang(. 张英逊. ). China Institute of Atomic Energy. The 11. th. International Conference on Nucleus-Nucleus Collisions, . 31May, NN2012, San Antonio, TX. and Other Applications: Hydrology +. Neutron Monitor Community Workshop—Honolulu, Hawaii . October . 24-25, 2015. Physicist. National Urban Security Technology Laboratory . Science and Technology Directorate. 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. To convert a percent into a decimal we will move the decimal point 2 places to the left and drop the percent sign.. Example:. Write 45.3% as a decimal:. 45.3 ⇨ 4.53 ⇨ .453. Converting From. 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. . 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 . Boris Pritychenko. 1. 1 National Nuclear Data Center, Brookhaven National. Laboratory, Upton, NY 11973-5000, USA. Heavy Elements Production in a Neutron Star Merger. Can we apply nuclear data libraries to address current astrophysical observations such as a multi-messenger signal from the NGC 4993 galaxy? . 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 . Stephen Croft (ORNL). Ramkumar Venkataraman (ORNL). Louise G. Worrall (ORNL). Robert D. McElroy Jr. (ORNL). Andrea Favalli (LANL). Acknowledgement. This work was sponsored in part by the U.S. Department of Energy (DOE), National Nuclear Security Administration (NNSA), Office of Defense Nuclear Nonproliferation Research and Development (NA-22) and in part by ORNL and LANL.. diesel to electric be . capitalized. or . expensed. ?. UPS converting diesel-fueled delivery vehicles . to be all-electric. In New York City, UPS is working on technology to convert 1,500 (66%) of its diesel-fueled delivery trucks to electric-fueled by 2020. 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...