Evolution of Pulsar Magnetic Fields

Because canonical neutron stars consist mainly of superfluid neutrons, superconducting protons and extremely relativistic electrons, all enclosed by a thin solid crust, the magnetic field structures of these stars vary in predictable ways during stellar spin-up and spin-down. Predicted consequences will be compared to a variety of observations of regular and millisecond pulsars including sudden changes in pulsar spin-periods ("glitches") and very slow oscillations of them ("precession"?).

 

Date: 
18/05/2001 - 14:00
Speaker: 
Prof. Malvin Ruderman
Filiation: 
Instituto de Astrofísica de Andalucía - CSIC


Seminars