PPT-Dynamics of superfluid-superconducting neutron stars

Mikhail E Gusakov Vasiliy A Dommes Ioffe Institute SaintPetersburg Russia Introduction It is generally accepted that baryons neutrons and protons in the internal layers of neutron stars undergo transition into superfluidsuperconducting state at . 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. Richard Kouzes. Ken Conlin, James Ely, Luke Erikson, Azaree Lintereur, Emily Mace, Edward Siciliano, Daniel Stephens, David Stromswold, Renee Van Ginhoven, Mitch Woodring. Pacific Northwest National Laboratory. 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. 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. Stars born with more than 8 — 10 M.  . cannot . lose enough mass to become white dwarfs. . These stars die by supernova explosions.. Ignition of “metals”. The core of an old high-mass star gets little . Robert McGreevy. Deputy Director. Neutron Sciences Directorate. May 3. rd. 2012. Oak Ridge Neutron Sciences . Operate two world class neutron facilities. Carry . out world class research. Enable . an outstanding User Science Program . Theory & Observations. Hovik Grigorian. Yerevan State University. Summer School Dubna – 2012. Compact stars Physics. • physics of compact stars,. • astrophysics of compact stars,. • . 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 . superfluid. neutron stars. Elena Kantor. , . Mikhail . Gusakov. Ioffe. Institute. Rotating NSs support inertial oscillation modes, in particular r-modes, which are subject to gravitational-driven instability at . NewCompStar. . Budapest. , 19.06.2015. M. Ali Alpar. ongoing. . work. . with. Onur Akbal . and. . Erbil. . Gügercinoğlu. *. Overview. on . glitches. : . External. . torque. , . starquakes. Design work at LLNL . Matthew Horsley, . LLNL. Workshop . on Microwave Cavity Design for . Axion. Detection. Tuesday. , August 25, 2015 . Outline. Introduction. Design Considerations. Simulation. Introduction. Stephen Hawking - The Birth of Stars - YouTube. Life Cycle of Stars. Nebula – large cloud of gas and dust spread out in an immense volume. Life Cycle of Stars. Gravity pulls gas and dust together in the densest part of the nebula. Magnetic Field. While MRI is considered to be a safe imaging technique, it is not without hazards. The magnet field will attract many ferromagnetic metals in an uncontrolled fashion and cause them to fly towards the magnets bore and turning them into high velocity projectiles. The bore of the magnet is where the fringe field is strongest, as all the lines of force are constricted and their relative strengths heightened. Various objects can be considered projectiles. 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 .