Transcript Stellar Evolution

Stellar Evolution
Where do gold earrings come from?
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Concept Test
• Order the
clusters from
youngest to
oldest.
a. DBCA
b. ACBD
c. DCBA
d. ADBC
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The Main Sequence
• A star is a delicate
balance between the
force of gravity
pulling in, and
pressure pushing
out.
• Stars on the main
sequence fuse
hydrogen in their
core to produce
thermal pressure.
• Longest phase of a
star’s life.
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What then?
• When the hydrogen in the core is almost consumed the
balance between gravity thermal pressure pushing out and
gravity pushing in is disturbed.
• The structure and appearance of the star changes
dramatically.
• What happens then, depends on the star’s mass.
• Two cases:
– Low-mass (< 8 x mass of Sun)
– High-mass (> 8 x mass of Sun)
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Helium
Ash
• Heavier elements, sink to the “bottom.”
• After 10 billion years, core is “choked” with helium “ash”.
• H  He continues in shell around non-burning core.
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The Red Giant Branch
• Without fusion pressure in
core:
– Helium core collapses (no
counter to gravity)
– Density in core increases.
• 3He  C + Energy in core
• 4H  He + Energy in shell
• Extra energy results in extra
pressure. Star expands.
• The star gets bigger while its
outside gets cooler.
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The Onion Sun
• Red Giant Stars
• Layers of:
–
–
–
–
Non-fusing H
Fusing H
Fusing He
Non-fusing C “ash”
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Red Supergiant
• What happens when the
Sun runs out of helium in
its core?
• Same as before.
• Core shrinks, surface
expands.
• Radius ~ 3 AU!
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Death
• Core is contracting and heating.
– Surface is cooling and expanding.
• Will it finally become hot enough in core for Carbon to
fuse?
• For the Sun: No.
• Gravity keeps contracting the core: 1000 kg/cm3!
• What stops it?
• Electron degeneracy pressure!
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Electron Degeneracy
Pressure from motion of atoms
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Electron Degeneracy
Pressure from electron shells
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NGC3242 – HST – Bruce Balick
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M57 – Ring Nebula
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M27 – Dumbbell Nebula – copyright VLT, ESO
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Cat’s Eye
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Eskimo Nebula
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Hourglass Nebula
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White Dwarf
• Mass of Sun
• Radius of Earth
• Hot as Sun’s core
• A million times denser than lead
• Slowly cool off
NGC2440 – HST – Bruce Balick
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High-Mass Stars
• Think back to the first
carbon core.
• How they get from main
sequence to the carbon
core stage is a little
different.
• Now however, there is
enough mass that it
becomes hot enough to
fuse carbon?
• Hot enough to eventually fuse lots of elements.
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The Iron Core
4H  He + Energy
3He  C + Energy
C + He  O + Energy
The ash of one reaction, becomes the fuel of the
next.
• Fusion takes place in the core as long as the end
result also yields energy.
• This energy causes pressure which counters
gravity.
• But Iron doesn’t fuse.
•
•
•
•
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Core-Collapse
•
•
•
•
•
•
Iron core – no outward pressure.
Gravity wins!
Star collapses rapidly!
Electron degeneracy can’t stop it.
Atomic structure can’t stop it.
Electrons and protons crushed together to produce
neutrons.
• Neutrons pushed together by force of gravity.
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Supernova
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Supernova
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Supernova
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Supernova
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Supernova
• The result of the catastrophic collapse is the
rebound and explosion of the core.
• From start of collapse to now: 1 second!
• Matter thrown back into the interstellar medium.
• Matter rushing outwards, fuses with matter
rushing inwards.
• Every element after Fe is made in the instant of a
supernova!
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M1 – Crab Nebula – copyright VLT
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NGC 4526 – 6 Million parsecs away
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Concept Test
•
Which of the following lists, in the correct order,
a possible evolutionary path for a star?
a.
b.
c.
d.
e.
Red Giant, Neutron Star, White Dwarf, Nothing
Red Giant, White Dwarf, Black Hole
Red Giant, Supernova, Planetary Nebula, Neutron Star
Red Giant, Planetary Nebula, White Dwarf
Red Giant, Planetary Nebula, Black Hole
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Homework #12
• For 2/20:
• Read B18.3-18.5
• Do: Problems 16 and 18.
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