stellar remnants white dwarfs type ia supernovae …miller/astr100/class22.pdf · • this turns...
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Today
Stellar Remnants
White Dwarfs
Type Ia Supernovae
Neutron Stars
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Reminder: Next Homework
• The next homework is due the Tuesday after Thanksgiving
• Necessary so we can squeeze in a last homework at the end of class
• I strongly recommend that you start now, so that you don’t have to think about it during your break!
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Dead Stars leave corpses• White dwarfs
– remnant core of low mass star– supported by electron degeneracy pressure
• Neutron stars– remnant core of high mass star– supported by neutron degeneracy pressure
• Black Holes– remnant of some massive stars– gravity’s ultimate victory
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White Dwarfs• White dwarfs are
the remaining cores of dead stars.
• Electron degeneracy pressure supports them against gravity.
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White dwarfs cool off and grow dimmer with time.
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Electron Degeneracy
• A white dwarf is the spent fuel of a stellar core. Fusion has ceased. What holds it up?
• Electron degeneracy– gravity crushes atoms as close together as
possible, so that the electrons “bump” into each other.
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Electron Degeneracy• Electron degeneracy pressure is really a
quantum mechanical effect stemming from the Heisenberg Uncertainty Principle:
• The position x of the electrons becomes very confined, so their momentum p - and in sum, their pressure - becomes large.
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∆x∆p ≥ �/2
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M < 1.4 M⊙
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9Mass
Rad
ius
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n se
quen
ce st
ars
browndwarfsJu
pite
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mass-radius relationfor normal stars
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Size of a White Dwarf
• White dwarfs with the same mass as the Sun are about the same size as Earth.
• Higher-mass white dwarfs are smaller.11
Diamond
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White Dwarf Density
• size R ~ thousands of kilometers• mass M ~ mass of stars• density absurdly high:
– white dwarf matter is roughly a million times denser than water
– instead of weighing a gram, an ice cube block of white dwarf material would weigh a ton.
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The White Dwarf Limit
• Quantum mechanics says that electrons must move faster as they are squeezed into a very small space
• As a white dwarf’s mass approaches 1.4MSun, its electrons move at a speed approaching that of light.
• This turns out to make the white dwarf unstable; it starts contracting and keeps contracting faster and faster, almost at free fall!
• This is also what allows the cores of massive stars to collapse and lead to massive star supernovae
• Thus white dwarfs cannot be more massive than 1.4MSun, the white dwarf limit (also known as the Chandrasekhar limit).
• more commonly known as the Chandrasekhar limit
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Limiting mass14
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White dwarf in a close binary
Roche lobes:over/undersurface where the gravity of two stars balance.
What happens if you add mass to a white dwarf?
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Accretion Disks• Mass falling toward
a white dwarf from its close binary companion has some angular momentum.
• The matter therefore orbits the white dwarf in an accretion disk.
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Accretion Disks• Friction between
orbiting rings of matter in the disk transfers angular momentum outward and causes the disk to heat up and glow.
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Nova• The temperature of
accreted matter eventually becomes hot enough for hydrogen fusion.
• Fusion begins suddenly and explosively on the surface of a white dwarf, causing a nova. 18
Demo
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Nova• The nova star
system temporarily appears much brighter.
• The explosion drives accreted matter out into space.
Only the surface is affected... 19
Video
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Adding Matter to a WD
A.The WD simply gets heavier
B. The WD turns into a normal star
C. The WD collapses
D.The companion starts to take matter from the WD
E. I don’t know
Suppose a white dwarf in a binary is just below the Chandrasekhar limit, and more matter falls onto the
WD from the companion. What happens?
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Two Types of Supernova
Massive star supernova: Iron core of massive star reaches white dwarf limit and collapses into a neutron star, causing explosion
White dwarf supernova: Carbon fusion suddenly begins as white dwarf in close binary system reaches
white dwarf limit, resulting in total explosion...entire white dwarf is disrupted.
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Simulation
Very important in cosmology!
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One way to tell supernova types apart is with a light curve showing how luminosity changes with time.22
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Nova or Supernova?
• Supernovae are MUCH MUCH more luminous (about 10 million times) !!!
• Nova: – H to He fusion of a layer of accreted matter, white
dwarf left intact
• Supernova: – complete explosion of white dwarf, nothing left behind
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Supernova Type: Massive Star or White Dwarf?
• Light curves differ
• Spectra differ (exploding white dwarfs don’t have hydrogen absorption lines)– White dwarf supernova spectra lack hydrogen
• no exterior “unburnt” layers– Massive star supernova spectra have hydrogen
• most of outer star still unburnt 24
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A neutron star is the ball of neutrons left behind by a massive-star supernova.
The degeneracy pressure of neutrons supports a neutron star against gravity.
Neutron Stars
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1.4 < M < 3 M⊙
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Electron degeneracy pressure goes away because electrons combine with protons, making neutrons and neutrinos.
Neutrons collapse to the center, forming a neutron star.
Supported by neutron degeneracy pressure.
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A neutron star is about the same size as a small city -roughly 10 km. 29
From my webpagehttp://www.astro.umd.edu/~miller/nstar.html
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Neutron Star Density• size R ~ ten kilometers• mass M ~ mass of stars• density extra-absurdly high:
– equivalent to the entire mass of the earth being stuffed into this building, or all 7 billion people on Earth being jammed into a teaspoon!
density ! 1014 g cm!3
nuclear density
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Discovery of Neutron Stars
• Using a radio telescope in 1967, Jocelyn Bell noticed very regular pulses of radio emission coming from a single part of the sky.
• The pulses were coming from a spinning neutron star—a pulsar.
http://www.jb.man.ac.uk/~pulsar/Education/Sounds/sounds.html 31
Demo
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Pulsar at center of Crab Nebula pulses 30 times per second
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X-rays Visible light33
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PulsarsA pulsar is a neutron star that beams radiation along a magnetic axis that is not aligned with the rotation axis.
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PulsarsThe radiation beams sweep through space like lighthouse beams as the neutron star rotates.
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