PPT-Challenges in the Measurement of Neutron Star Radii

Cole Miller University of Maryland 1 Collaborators Romain Artigue Didier Barret Sudip Bhattacharyya Stratos Boutloukos Novarah Kazmi Fred Lamb Ka Ho Lo Outline. 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 . Magdalena Kowalska. CERN, PH-Dept.. kowalska@cern.ch. . below. Outline . 2. Laser spectroscopy on radioactive nuclei. Optical isotope shifts. A long way from isotope shifts to charge radii. Take-home message . Phil Rosenfield, . Fridolin. Weber, Horst . Lenske. Outline. Neutron stars: a short synopsis. The structure of neutron stars. Modeling neutron stars. The equation of state. . Rotating or non-rotating. . 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. A Year 2 Joint Hurricane . Testbed. Project Update. . Mark DeMaria. 1. , Robert DeMaria. 2. , Andrea Schumacher. 2. , . Daniel Brown. 3. , Michael Brennan. 3. , Richard Knabb. 4. , Pablo Santos. 5. and . GRBs structure. Alessandro Drago. University. of Ferrara. Outline. What. do . we. . learn. from the . existence. of . stars. of 2 . M. s. . ?. Are . hyperons. . excluded. ? . Are . hybrid. 1. What is an atom’s atomic radii?. 2. What happens to atomic radii across a period? Why?. 3. What happens to atomic radii as you move down a group? Why?. Practice problems, page 144. Ionization Energy. 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 . !W"0.05 γ-ray spectra in . fast neutron-induced fission. Brugge – ND 2016. J.-M. Laborie, . G. Bélier. , J. . Taieb CEA/DIF F-91297 Arpajon, France. A. . . Oberstedt. . Fundamental. . Fysik. , . Chalmers. 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. Rudy . Wijnands. Anton . Pannekoek. Institute for Astronomy. University of Amsterdam. 15 December 2015. Texas Symposium 2015, Geneva. X-. ray. . luminosity. Quiescence. Outburst. Low-mass X-ray binary transients. 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 .