PPT-Cocoons, structured jets, binary neutron star mergers, and GW170817

Davide Lazzati Oregon State University Rosalba Perna Stony Brook Brian J Morsony UMD Diego LópezCámara UNAM Matteo Cantiello CCA Princeton Riccardo Ciolfi. 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.. in Star Forming Region. Tae-. Soo. . Pyo. Subaru Telescope. Near-IR . NBFs. Survey of Jets in Massive Star Forming Region with GLAO. . Key words:. -. GLAO : FWHM ~ 0.2” , . FoV. ~ 15’x 15’. . 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. Steve Branson . Oscar . Beijbom. . Serge . Belongie. CVPR 2013, Portland, Oregon. . UC San Diego. . UC San Diego. . Caltech. Overview. Structured prediction . Learning from larger datasets. 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. Steve Branson . Oscar . Beijbom. . Serge . Belongie. CVPR 2013, Portland, Oregon. . UC San Diego. . UC San Diego. . Caltech. Overview. Structured prediction . Learning from larger datasets. 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’. are . relatively widely . separated. , . their . evolution proceeds much as it . would . have if they were not . companions.... If they are . closer. , it is possible for . material . to transfer from one star to another, . 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 . an overview. Matthew Pitkin . for the LVC. University of Glasgow. LIGO-DCC G1500072. Astronomy group seminar,. University . of Southampton, Jan 2015. Gravitational wave (GW) background. What are gravitational waves?. 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...