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.

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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 “Dark Tower” in Scorpius

The Pillars of Creation near Orion

Pleiades in Visible

light

Pleiades in IR light

“false” colors, applied to

match temperatures

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

Extinction nebulae from

gas/dust blocking light

Emission nebulae from gas emitting

light

Extinction nebulae from

gas/dust blocking light

Reflection nebulae from

dust scattering blue light

The Horsehead Nebula

Dust grains also cause “interstellar reddening”

Dust grains also cause “interstellar reddening”

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

Pleiades “Open”

Cluster in disk of Milky Way

Galaxy

Pleiades HR Diagram

Stars of all types & masses

Another Star Cluster

Stars of all types & masses

NGC 2264 HR Diagram

Some objects not yet formed

as stars!

“T-Tauri Protostars”

Observational evidence of “protostars”

Protostars seem to appear in CLUSTERS

New Stars & Brown Dwarfs that will never be…

An actual Brown Dwarf!

Supermassive stars lead very unstable lives!

Pressure from fusion literally blows outer layers away!

One of the largest stars

known….

5,000,000 times

brighter than our

Sun!

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

Disks & Jets in Protostars

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?

Star Formation in 4 Steps!

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

Low mass stars models predict mixing inside to convert all H to He

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!