astro chapter 21

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  1. accretion disk
    • formed in a white dwarf binary. Viscosity (friction) within the gas brings it down onto the white dwarfs surface, later forming a nova
    • creates visible, UV, and even the X-ray
  2. what causes a nova's decline in brightness
    expansion and cooling of the white dwarf's surface layers as they are blown into space
  3. neutronization
    in the core of a large mass star under collapse, protons and electrons are crushed together forming neutrons and neutrinons
  4. why does the supernova happen
    pressures get so high that neutrons touch, overshoots density and recoils, shooting out exploding the star (1,000km/s's)
  5. how much brighter is a supernova compared to a nova
    million times brighter
  6. type I supernoa
    • hydrogen poor
    • carbon collapse super nova
    • descendent of a lower mass star
    • white dwarf goes over its chandrasekhar mass limit, electron degeneracy can't hold pressure.
  7. what's the maximum mass of a white dwarf star
    • 1.4solar masses
    • chandrasekhar mass
  8. crab nebula
    supernova written in history books
  9. primordial
    • elements that date from the very earliest times
    • hydrogen and helium
  10. helium capture
    can build up to high elements more easily than like elements combining
  11. how do we form elements about iron
    neutron capture
  12. what type of elements do the youngest stars show
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astro chapter 21
2014-04-22 01:19:25

text chapter 21
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