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88
GoalsGoals
• What is there between the stars?• What are dust clouds?• What are nebulae?• How do these lead to the formation of
star?– Where do baby stars come from?
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The Stuff Between Stars
• Space isn’t empty.• Interstellar Medium – The gas and dust
between the stars.
All the interstellar gas and dust in a volume the size of the Earth only yields enough matter to make a pair of dice.
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The Distribution• Picture the dust under your bed.
– Fairly uniform thin layer– Some small clumps– Occasional big complexes
• Interstellar dust and gas is the same.
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Dust• Space is dirty.• Dust blocks or
scatters some light.• Result: black clouds
and patterns against the background sky.
• But what light gets through, and what light doesn’t?
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Absorption and Scattering
• Q: Why are sunsets red?• Light is absorbed or scattered by
objects the same size or smaller than its wavelength.
• Dust grains = wavelength of blue light• Dust clouds:
– Opaque to blue light, UV, X-rays– Transparent to red light, IR, radio
• A: Whenever there is a lot of dust between you and the Sun, the blue light is absorbed or scattered leaving the only the red light.
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Interstellar Reddening• Same thing with
dust clouds in space.
• Since space is full of dust, the farther away stars are, the redder they look.
• Enough dust and eventually all visible light is scattered or absorbed.
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Dust and IR• In a dark dust cloud:
– Even though all visible light may be gone, we can still use IR.
– If dust is warm, IR will show its blackbody emission.
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The IR Universe
And allows us to see dust where we wouldn’t otherwise expect it.
Orion - visible
Orion – by IRAS
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Interstellar Gas
• In Lab 2 we talked about spectral lines and how they apply to hot and cool gases.
• Let’s look at some hot and cool gases in space.
Hemission nebulae
Copyright - Jason Ware
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• In order for the hydrogen to emit light, the atoms must be in the process of being excited.
• The energy for the excitation comes from very hot stars (O and B stars) within the cloud.
Orion Nebula – copyright Robert Gendler
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Cold Dark Clouds• If dust clouds
block light, then inside thick dust clouds there should be no light at all.
• Without light, there is little energy.
• With little energy, any gas inside is very, very cold.
• Inside molecules can form.
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Gravity vs. Pressure
• Stars and other interstellar material are in a perpetual battle between forces pulling in (gravity) and forces pushing out (pressure).
• Gravity comes from the mass of the cloud or star.
• Pressure comes from the motion of the atoms or molecules.– Think of hot air balloons.– The hotter the air, the bigger the
balloon.
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Star Formation• Remember lecture 4:
• Cold interstellar clouds:No heat = no velocity = no outward pressure.Gravity wins.
• Gas begins to contract.
HOTTER COOLER
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1. The Interstellar Cloud
• Cold clouds can be tens of parsecs across.
• Thousands of times the mass of the Sun.
• Temperatures 10 – 100 K.• In such a cloud:
– Something makes a region denser than normal.
– Force of gravity draws material to denser region.
– Gravitational collapse begins.
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Contracting Fragments
• Cloud about the size of solar system.• In the center:
– Collapsing material continues to heat up.– Density causes heat to be retained.
• Higher density makes center opaque.
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2. Protostar
• The central opaque part is called a protostar.
• Mass increases as material rains down on it.
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Planetesimals• Dust and gas
condense onto dust grains.
• Small clumps grow bigger.
• Bigger clumps have more mass and attract more matter.
• Planetesimals become the building blocks of the planets.
Orion Nebula – Copyright O’Dell and Wong
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3. T Tauri Phase• Protostar still shrinks: 10x
the Sun.• Still heats up: surface =
4000 K• Core temp = 5,000,000 K• Violent surface activity
creates strong winds that blow material away near the protostar’s surface.
• Clear away the dust and gas between planets.
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A Star is Born
• Time: 40- 50 million years since the collapse started.
• Radius: 1,000,000 km (Recall the Sun = 700,000 km)
• Core temp: 10,000,000 K (Sun = 15,000,000 K)– Surface temp = 4500 K
• Fusion begins in core.• Energy released creates the pressure needed
to counter the contraction from gravity.• Contraction ends!
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The Main Sequence
• For the Sun:– While it took 40 – 50
million years to get here, the new star will spend the next 10 billion years as a main sequence star.
• Bigger Stars:– Everything goes
quicker.
• Smaller Stars:– Everything longer.
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Now what?• The mass of the
star that is formed will determine the rest of its life!
• Recall: the more massive the star, the more pressure in the core.
• The more pressure, the more fusion.
• More fusion:– More energy
produced– Hotter– Shorter life span
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Open Clusters
• These are the new stars.
• Small groups of young stars.
• Slowly drifting apart.
Jewel Box – copyright MichaelBessell