PPT-How Well Can We Measure 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 Measuring stellar radii. X-ray binaries. Rudy . Wijnands. Anton . Pannekoek. Institute for Astronomy. University of Amsterdam. 3 August 2015. Lorentz center, Leiden. Low- versus high-mass X-ray binaries. Low-mass X-ray binaries. 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 . and Other Applications: Hydrology +. Neutron Monitor Community Workshop—Honolulu, Hawaii . October . 24-25, 2015. Physicist. National Urban Security Technology Laboratory . Science and Technology Directorate. 48. Ca. INTC-P-313. M.L. Bissell - On behalf of COLLAPS . Background.  .  . Program initiated with IS-484 - . “. Ground-state properties . of . K-isotopes from laser and . β. -NMR . spectroscopy. 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. What is the difference between a Bohr models, Lewis Dot Diagram, and the Nuclear Symbol? . 1. Periodicity . Periodic Trends . 2. Periodic Law . The chemical and physical properties of the elements are periodic functions of their atomic numbers; properties of the elements occurred at repeated intervals called periods.. 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’. 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. !W"0.05 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...