evolution of high mass stars
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Evolution of High Mass Stars. AST 112. High Mass Stars. So… what exactly do high mass stars do? The same thing as low mass stars: they get on the Main Sequence and convert H to He. Then they blow up!. Life From Stars. Need low mass stars for life - PowerPoint PPT PresentationTRANSCRIPT
High Mass Stars
• So… what exactly do high mass stars do?
• The same thing as low mass stars: they get on the Main Sequence and convert H to He.
• Then they blow up!
Life From Stars
• Need low mass stars for life– They live long enough to allow life to flourish
• Need high mass stars for life– They produce the elements heavier than carbon
High Mass Stars: Main Sequence
• Low mass stars fuse H into He through the proton – proton chain– Slow!
• High mass stars fuse H into He through the CNO cycle– Fast!
The CNO Cycle
• Recall that nuclear reactions happen when nuclei have enough kinetic energy to overcome electric repulsion
• High mass stars heat the cores to a higher temperature– H nuclei can now react with carbon, oxygen and
nitrogen
The CNO Cycle
• Carbon, nitrogen and oxygen act as catalysts– C, N, and O don’t get
consumed; they just “help out”
• This is why high mass stars shine bright and die young.
The CNO Cycle
• Text, Page 574:
Did the first high-mass stars in the history of the universe produce energy through the CNO cycle?
Hydrogen Exhaustion
• 25 MSun star uses up its hydrogen in a few million years
• Quickly develops a hydrogen burning shell, outer layers expand
• Helium gradually begins to burn (no helium flash)
Burning Helium
• Star burns He for few hundred thousand years
• Runs out of He– Inert carbon core begins collapse
• Similar to low-mass star thus far
Burning Carbon
• High-mass stars: HOT!– Easily reach 1,200,000,000 oF for carbon fusion
• Fuses carbon for a few hundred years, runs out
He-Capture Reactions
• Helium nucleus fuses with heavier nuclei
– Carbon to Oxygen
– Oxygen to Neon
– Neon to Magnesium
Helium Capture Reactions
Heavy Nucleus Reactions
• In the core:
– Carbon + Oxygen -> Silicon
– Oxygen + Oxygen -> Sulfur
– Silicon + Silicon -> IronHeavy-Nucleus Reactions
Advanced Nuclear Burning
• The core fuses elements, runs out, shrinks, heats, and fuses new elements
• This results in layers of heavy elements
High Mass Stars: Advanced Nuclear Burning
• These sequential shells result in a zig-zag path about the HR diagram
• Most massive stars: outer layers don’t have time to respond!
High Mass Stars: Advanced Nuclear Burning
• Iron starts to accumulate in the central core
– Elements lighter than iron release energy when fused
– Elements heavier than iron release energy when split
High Mass Stars: Advanced Nuclear Burning
• Not energetically advantageous for iron to fuse / split
…so it doesn’t.
High Mass Stars: Advanced Nuclear Burning
• Iron is not undergoing nuclear reactions
• Doesn’t collapse – Electron degeneracy pressure (cramming too
much stuff together)
• Iron keeps on piling up…
Death of a High Mass Star
A good way to remove electron degeneracy pressure:
Get rid of the electrons!
Death of a High Mass Star
• … and piling up and piling up…
• Conditions such that electrons combine with protons– Forms neutrons, releases
neutrinos– Degeneracy pressure
vanishes instantly
Death of a High Mass Star
In a split second, an iron core the size of Earth collapses into a sphere of
neutrons 5-10 miles across and releases a torrent of neutrinos.
This releases 100x the energy released by our Sun in its entire
lifetime!
Supernova
• Outer layers of the star get blown away– Mostly due to neutrinos– 6000 miles / second • (3% speed of light!)
• The leftover core is either:– A neutron star if it’s small enough– A black hole if it’s large enough
Supernova
• A supernova is so bright it can briefly outshine an entire galaxy!
• Bright for about a week, fades over months
Neutron-Capture Reactions
• Where do elements heavier than iron come from?
• Rare reactions that capture a neutron– Neutron changes to proton– Repeats
• Requires high energy– Only happens close to and during supernova
Nuclear Reactions: Observational Evidence
• Look at composition of stars, gas, dust in Milky Way
• Look at C, O, or Ne– Even number of protons– Come from He capture (+2
protons)– These can fuse together
• Elements heavier than iron are rare
Notorious Supernova Remnants
• Messier 1, The Crab Nebula (in Taurus)
• Growing several thousand miles per second!
• Neutron star lives inside
Notorious Supernova Remnants
• Re-tracing the Crab Nebula’s expansion puts the supernova at 1100 A.D.
In the first year of the period Chih-ho,the fifth moon, the day chi-ch’ou, a guest star appeared approximately several[degrees] southeast of Thien-kuan. After more than a year it gradually becameinvisible.
July 4, 1054
Taurus
Notorious Supernova Remnants
• Supernova 1987A occurred in the Large Magellanic Cloud
• 150k LY away– Did the star explode in
1987?
Milky Way Supernovas
• Four in the last 1000 years:
– 1006 (So bright it cast shadows at night!)– 1054 (Just did that one)– 1572 (Tycho Brahe saw it)– 1604 (Kepler saw it)
Betelgeuse
• The size of the star extends out past the orbit of Mars
• Its shape is pulsating
• 600 LY away… it’s safe.