Black holes, white dwarfs, and neutron stars Saul A. Teukolsky, Stuart L. Shapiro
Publisher: John Wiley & Sons Inc

A star undergoes many radical changes throughout its lifespan including the inevitable exhaustion of its fuel source. They are extremely massive stars with a strong force of gravity. When stars die, the distribution of remnant masses would be expected to be continuous from white dwarfs through neutron stars to black holes, ranging from a fraction of our sun's mass to nearly 100 solar masses. For those with serious interest in neutron stars and other compact objects, an excellent reference is "Black Holes, White Dwarfs, and Neutron Stars", by Stuart Shapiro and Saul Teukolsky (1983, John Wiley and Sons). Our Sun is expected to end as a white dwarf after it is a red giant. White dwarfs are the hot, dense leftover cores of ex-stars. Black holes, white dwarfs, neutron stars and quasars emit an extremely strong, pulsing beam of Light, which is made up of the spectrum of Light waves that include Ultra-Violet. An exhausted star will evolve into a neutron star, a black hole or a white dwarf – depending on its mass. Lectures will be presented by leading Physicists and Astrophysicists working in the interface of Nuclear Physics, White Dwarfs, Neutron Star Physics and Black Holes Physics. Michael Muno is an astrophysicist who uses Chandra, among other telescopes, to study some of the most exotic objects in the Universe: white dwarfs, neutron stars, and black holes. In addition, many binary systems can have compact components and can exist in a variety of ways. We look at the skies and see stars at various stages of their evolution — young ones, middle aged ones, supernovas, and the remnants of supernovas — white dwarves, neutron stars, black holes. We can't hope to create extremely strong gravity in the lab, so we need to look outwards into space for things like black holes, neutron stars and white dwarfs.