1 To Be or Not to Be: The Mysteries of Disk Formation Around Rapidly Spinning Be Stars Douglas R. Gies Department of Physics and Astronomy Center for High.
THE CANNONBALL MODEL AND SHORT HARD BURSTS Arnon Dar 44 th Rencontre De Moriond, La Thuile, Italy, February 1-8, 2009 Based on work done in collaboration.
Understanding the Evolution of Close Binary Systems With Radio Pulsars
Magnetars: SGRs and AXPs. Magnetars in the Galaxy ~7 SGRs, ~12 AXPs, plus candidates, plus radio pulsars with high magnetic fields (about them see arXiv:
Chapter 21 Stellar Explosions. 21.1Life after Death for White Dwarfs 21.2The End of a High-Mass Star 21.3Supernovae Supernova 1987A 21.4The Formation.
Magnetars: SGRs and AXPs. Magnetars in the Galaxy ~11 SGRs, ~12 AXPs, plus candidates, plus radio pulsars with high magnetic fields (about them see arXiv:
1. accretion disk - flat disk of matter spiraling down onto the surface of a star. Often from a companion star.
Stellar Explosions. Introduction Life after Death for White Dwarfs The End of a High-Mass Star Supernovae Supernova 1987A The Crab Nebula in Motion The.
1. White Dwarf If initial star mass < 8 M Sun or so. (and remember: Maximum WD mass is 1.4 M Sun, radius is about that of the Earth) 2. Neutron Star If.
What is Dark Energy? Josh Frieman Fermilab and the University of Chicago.
1 TORAH LIGHT MINISTRIES P.O. Box 2500 OROVILLE WA 98844 The SIGN and the Flood: Lesson #4.
What is Dark Energy?
