Chapter 14

Chapter 14 - Note that the following lectures include...

Info iconThis preview shows pages 1–11. Sign up to view the full content.

View Full Document Right Arrow Icon
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode).
Background image of page 1

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Neutron Stars and Black Holes Chapter 14
Background image of page 2
The preceding chapters have traced the story of stars from their birth as clouds of gas in the interstellar medium to their final collapse. This chapter finishes the story by discussing the kinds of objects that remain after a massive star dies. How strange and wonderful that we humans can talk about places in the universe where gravity is so strong it bends space, slows time, and curves light back on itself! To carry on these discussions, astronomers have learned to use the language of relativity. Throughout this chapter, remember that our generalized discussions are made possible by astronomers studying general relativity in all its mathematical sophistication. That is, our understanding rests on a rich foundation of theory. This chapter ends the story of individual stars. The next three chapters, however, extend that story to include the giant communities in which stars live— the galaxies. Guidepost
Background image of page 3

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
I. Neutron Stars A. Theoretical Prediction of Neutron Stars B. The Discovery of Pulsars C. A Model Pulsar D. The Evolution of Pulsars E. Binary Pulsars F. The Fastest Pulsars G. Pulsar Planets II. Black Holes A. Escape Velocity B. Schwarzschild Black Holes C. Black Holes Have No Hair D. A Leap into a Black Hole E. The Search for Black Holes Outline
Background image of page 4
III. Compact Objects with Disks and Jets A. X-Ray Bursters B. Accretion Disk Observations C. Jets of Energy from Compact Objects D. Gamma-Ray Bursts Outline (continued)
Background image of page 5

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Neutron Stars The central core will collapse into a compact object of ~ a few M sun . A supernova explosion of a M > 8 M sun star blows away its outer layers.
Background image of page 6
Formation of Neutron Stars Compact objects more massive than the Chandrasekhar Limit (1.4 M sun ) collapse further. Pressure becomes so high that electrons and protons combine to form stable neutrons throughout the object: p + e - n + ν e Neutron Star
Background image of page 7

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Properties of Neutron Stars Typical size: R ~ 10 km Mass: M ~ 1.4 – 3 M sun Density: ρ ~ 10 14 g/cm 3 Piece of neutron star matter of the size of a sugar cube has a mass of ~ 100 million tons!!!
Background image of page 8
Discovery of Pulsars => Collapsing stellar core spins up to periods of ~ a few milliseconds. Angular momentum conservation => Rapidly pulsed (optical and radio) emission from some objects interpreted as spin period of neutron stars Magnetic fields are amplified up to B ~ 10 9 – 10 15 G. (up to 10 12 times the average magnetic field of the sun)
Background image of page 9

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Wien’s displacement law, λ max = 3,000,000 nm / T[K] gives a maximum wavelength of λ max = 3 nm, which corresponds to X-rays. Cas A in X-rays
Background image of page 10
Image of page 11
This is the end of the preview. Sign up to access the rest of the document.

Page1 / 66

Chapter 14 - Note that the following lectures include...

This preview shows document pages 1 - 11. Sign up to view the full document.

View Full Document Right Arrow Icon
Ask a homework question - tutors are online