Abstract: I will discuss MHD for superconducting protons in neutron stars with remarks on various issues: 1. free energy of the superconductor; 2. magnetic force density (not just Lorentz); 3. requirements for MHD fluid equilibria; 4. how boundary conditions determine the surface magnetic field strength for the “most dipolar field” in terms of neutron star equation of state; 5. magnetic distortions; 6. an instability you may not know about, and others you do; 7. a more sophisticated treatment of primarily toroidal fields; 8. implications for neutron star spin dynamics.
My Unhealthy Obsession with Cylinders
Ira Wasserman (Cornell) // June 1, 2015
Abstract: I will discuss MHD for superconducting protons in neutron stars with remarks on various issues: 1. free energy of the superconductor; 2. magnetic force density (not just Lorentz); 3. requirements for MHD fluid equilibria; 4. how boundary conditions determine the surface magnetic field strength for the “most dipolar field” in terms of neutron star equation of state; 5. magnetic distortions; 6. an instability you may not know about, and others you do; 7. a more sophisticated treatment of primarily toroidal fields; 8. implications for neutron star spin dynamics.