1 / 17

Death of Stars II

Death of Stars II. Physics 113 Goderya. Chapter(s): 14 Learning Outcomes:. Neutron Stars. A supernova explosion of a M > 8 M sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M sun. Formation of Neutron Stars.

china
Télécharger la présentation

Death of Stars II

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Death of Stars II Physics 113 Goderya Chapter(s): 14 Learning Outcomes:

  2. Neutron Stars A supernova explosion of a M > 8 Msun star blows away its outer layers. The central core will collapse into a compact object of ~ a few Msun.

  3. Formation of Neutron Stars Compact objects more massive than the Chandrasekhar Limit (1.4 Msun) collapse further. Pressure becomes so high that electrons and protons combine to form stable neutrons throughout the object: p + e-n + ne Neutron Star

  4. Properties of Neutron Stars Typical size: R ~ 10 km Mass: M ~ 1.4 – 3 Msun Density: r ~ 1014 g/cm3 Piece of neutron star matter of the size of a sugar cube has a mass of ~ 100 million tons!!!

  5. Discovery of Pulsars Angular momentum conservation => Collapsing stellar core spins up to periods of ~ a few milliseconds. Magnetic fields are amplified up to B ~ 109 – 1015 G. (up to 1012 times the average magnetic field of the sun) => Rapidly pulsed (optical and radio) emission from some objects interpreted as spin period of neutron stars

  6. Pulsars / Neutron Stars Neutron star surface has a temperature of~ 1 million K. Cas A in X-rays Wien’s displacement law, lmax = 3,000,000 nm / T[K] gives a maximum wavelength of lmax = 3 nm, which corresponds to X-rays.

  7. Pulsar Periods Over time, pulsars lose energy and angular momentum => Pulsar rotation is gradually slowing down.

  8. Lighthouse Model of Pulsars A Pulsar’s magnetic field has a dipole structure, just like Earth. Radiation is emitted mostly along the magnetic poles.

  9. Neutron Star (SLIDESHOW MODE ONLY)

  10. Images of Pulsars and Other Neutron Stars The vela Pulsar moving through interstellar space The Crab nebula and pulsar

  11. The Crab Pulsar Pulsar wind + jets Remnant of a supernova observed in A.D. 1054

  12. The Crab Pulsar (2) Visual image X-ray image

  13. Light Curves of the Crab Pulsar

  14. Proper Motion of Neutron Stars Some neutron stars are moving rapidly through interstellar space. This might be a result of anisotropies during the supernova explosion forming the neutron star

  15. Binary Pulsars Some pulsars form binaries with other neutron stars (or black holes). Radial velocities resulting from the orbital motion lengthen the pulsar period when the pulsar is moving away from Earth... …and shorten the pulsar period when it is approaching Earth.

  16. Neutron Stars in Binary Systems: X-ray Binaries Example: Her X-1 Star eclipses neutron star and accretion disk periodically 2 Msun (F-type) star Neutron star Orbital period = 1.7 days Accretion disk material heats to several million K => X-ray emission

  17. Pulsar Planets Some pulsars have planets orbiting around them. Just like in binary pulsars, this can be discovered through variations of the pulsar period. As the planets orbit around the pulsar, they cause it to wobble around, resulting in slight changes of the observed pulsar period.

More Related