star stuff joy harjo (1951 – ) from secrets from the center of the world i can hear the sizzle of...
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Star Stuff
Joy Harjo (1951 – ) from Secrets From the Center of the World
I can hear the sizzle of newborn stars, and know anything of meaning, of the fierce magic emerging here. I am witness to flexible eternity, the evolving past, and know I will live forever, as dust or breath in the face of stars, in the shifting pattern of winds.
WHAT DO YOU THINK?
1. How do stars form?
2. Are stars still forming today? If so, where?
3. Do more massive stars shine longer than less massive ones? What is the reason?
Key Questions to Answer!
What is the interstellar medium made of? How do stars form? How do we know?
How will our Sun evolve as a star? What will its final state be? Compare its predicted evolution to that of higher-mass stars. How do they end? How do we know?
The Inter-stellar MediumObserve/Research
Where do stars form? What are they made of?What properties are common? Rare?
Create THEORY of star formation
Test hypotheses predicted by the theory
The ISM: How do we know?Where do stars form?
Visible, IR, Microwave, Radio observations
What are they made of?Spectra
What properties are common? Rare?HR Diagram, Mass, Number density, Location
Test hypotheses predicted by theoryVisible, IR, Microwave, Radio observations
ISM: Where do stars form?
We observe:
Visible “extinction nebulae” block background light
Visible emission nebulae form hot gas
Visible signs of dust scattering and dimming and reddening starlight
Learning About Stellar LivesHow can we know anything?
Create HR diagrams of clusters of stars
AssumeSame relative distance comparing relative brightness
is fair
Same relative age comparing masses and types of stars is fair
Supermassive stars lead very unstable lives!
Pressure from fusion literally blows outer layers away!
Star Formation in 4 Steps!
Start with Large Cloud of Gas & Dust
1. Shock creates fragments & “blobs”
2. Gravity creates clusters of star “seeds”
3. Individual blobs heat up and glow as protostars
4. Protostars start fusion in cores
5. ♫ A star is born!♫
Star Formation in 4 Steps!
Start with Large Cloud of Gas & DustGiant molecular cloudsRaw materials to form 100’s, 1000’s, or millions
of stars in clusters.Mass & Location affect # of stars to be formedTemperature affects rate of formation
Observations supporting this phase:Radio telescopes, Microwave Maps
Star Formation in 4 Steps!
1. Shock the cloud – break it into fragmentsGravitational Forces (galaxies, mergers,
collisions)Stellar winds of new massive starsSupernovae of massive stars that form fast
Observations supporting this phase:HST views of Eagle Nebulae
Star Formation in 4 Steps!
2. Gravity takes over, creating clusters of what will eventually be stars OB AssociationsOpen ClustersGlobular Clusters
Observations supporting this phase:Microwave/IR observations of warming regions
Star Formation in 4 Steps!
3. Individual blobs heat up, rotate, and glow as protostars
Contracting into disks Shining by gravitational energy (not fusing!) Larger than “real” stars, & cooler Develop jets of radiation from poles
Observations supporting this phase:T-Tauri stars
Star Formation in 4 Steps!
4. A star is born! Fusion of Hydrogen to Helium starts in core Stops Contracting Hydrostatic Equilibrium Established A “main sequence” star
But….
Will it have planets?
Lives of Main Sequence Stars
Where a star is plotted depends on mass
O dwarfs (O V) are most massiveM dwarfs (M V) are least massive
ALL Main Sequence stars fusing H He
Lives of Main Sequence Stars
ALL Main Sequence stars fusing H He
The star is stable, in balance
Gravity (in) vs. force (out) from gas pressure and radiation pressure from fusion reactions
Stellar Evolution
Building models of what happens to stars
Low mass (0.08 to 0.4 Msun
Medium mass (0.4 to 4+ Msun
Higher Mass (5+ to >100 Msun
Low mass star evolution (~8% to ~40% of our Sun’s Mass)
Slower fusion reaction rate
Cooler surface temp (red stars)
Low Luminosity
Longer Lives“Economy models!”
Low mass star evolution models
Totally “convective” inside! (mixed throughout)
convert ALL Hydrogen into Helium
don’t develop a Helium “core”
Eventually collapse to white dwarf
Medium Mass40% to 400% of Sun’s Mass
Life like our Sun – about 10 Billion years
Slowly develop Helium core Helium “ash” not fusing --- yet!
Surrounded by Hydrogen still fusing
Medium Mass40% to 400% of Sun’s Mass
Core collapses, becomes “degenerate”
Star swells into Red Giant
Eventual Helium FLASH as fusion of He Carbon starts up!
A “new” life– for a short time!
High Mass Stellar Evolution
Much greater fusion rate, MUCH brighter, MUCH, MUCH shorter lived stars
Quickly reach Helium Core stage, and can start fusing He Carbon, develop C core, then repeat with heavier and heavier atoms
High Mass Stellar Evolution
“Onion Skin” model of heavier & heavier shells
Fuse until Iron core formed…
Boom!