AST 1002 Lecture Notes - Lecture 14: Gravitational Wave, Accretion Disk, Flashlight
Document Summary
In 1967, a 24 year old graduate student (jocelyn bell) measured this radio signal from an unresolved source. Type ii supernova: core bounce in dying high mass stars. Just before the bounce, neutronization of the iron core occurs. No more iron or atoms or ions, just a ball of neutrons at nuclear densities. The bounce disrupts the rest of the star, not the neutron core a neutron star (leftover after the explosion) Composition: neutrons, mass: 1-3 msun, radius: 10 km (6 miles), density: 10^11 kg. cm^3. Spin very rapidly because of the conservation of angular momentum. Before collapse, normal stars rotate once per 25 days. Neutron stars rotate in less than a second. Neutron stars have very strong magnetic fields. Why: contracting stars carry the magnetic field with them, tiny neutron stars have very intense magnetic fields. A neutron star can be a pulsar. Tro(cid:374)g (cid:373)ag(cid:374)eti(cid:272) fields lead to (cid:862)hot spots(cid:863) at the (cid:373)ag(cid:374)eti(cid:272) poles: 2.
