ASTRON 2B03 Lecture Notes - Dim Stars, Main Sequence, Supermassive Black Hole

• School: McMaster University
• Department: Astronomy
• Course: ASTRON 2B03
• Professor: Laura Parker

Document Summary

Once you pass event horizon, you would have to accelerate to a speed greater than c to escape. Tidal forces (differential forces) force on feet different than force on head spaghetti. Larger black holes don"t necessarily get stretched. Because of effects of td and gr, you don"t see anything fall inside a black hole. Last photons we see, infinitely time dilated: closer to event horizon, blows up to infinity. We never see anything close to the scale of the event horizon. We see material close to the black hole -> many swarchild radii away. Really hot gas emits x ray radiation. Systems with orbits good place to look for black holes. If you see stars orbiting something, but cant see anything, it might be a black hole, especially if its orbiting quite strongly. If a black hole is close to the companion star, it is possible that it can strip the outer layer of gas of the star.