PPT-Neutron Star Environment:

from Supernova Remnants to Pulsar Wind Nebulae Stephen CY Ng McGill University Special thanks to Pat Slane for some materials in this talk Jun 21 2010 HKU Fermi Workshop Outline SNRs and . 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.. Nathalie . Degenaar. . University of Michigan. X-ray observations. Interior properties. Thermal evolution. Neutron stars . in transient X-ray binaries. Quiescence. :. No/little accretion. Faint X-ray emission. The Pulsar Search Collaboratory. Questions We Will Answer. What is a . pulsar. ?. Why do astronomers study pulsars?. What is the . PSC. ?. How can . you. get involved?. What is a pulsar?. A pulsar is a . 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. 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. Stars:. . The Discovery of . Pulsars. . Can. We Detect . Neutron Stars?. As noted earlier, . this . seems. very unlikely:. . they are small (asteroid-sized. ). even the nearest is likely to be . N. eutron . Stars Foreseen. . Supernova . End Products?. When a . supernova. goes off, we can speculate that:. The star might blow itself to smithereens, . scattering all its material into space and leaving . 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’. !W"0.05 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. 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...