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The Interstellar Medium. No, it’s not a space psychic. Goals. What is the interstellar medium? What are dust clouds? What are nebulae? How do these lead to the formation of star? Where do baby stars come from?. The Stuff Between Stars. Space isn’t empty.

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the interstellar medium

The Interstellar Medium

No, it’s not a space psychic

goals
Goals
  • What is the interstellar medium?
  • What are dust clouds?
  • What are nebulae?
  • How do these lead to the formation of star?
    • Where do baby stars come from?
the stuff between stars
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.

the distribution
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.
slide5
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?
absorption and scattering
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.
interstellar reddening
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.
dust and ir
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.
scattered light
Scattered light
  • Q: But what happens to the blue light that is scattered?
  • A: Reflection nebulae.

The Witchhead Nebula

interstellar gas

Haemission nebulae

Copyright - Jason Ware

Interstellar Gas
  • In lecture 2B we talked about Kirchhoff’s laws and how they apply to hot and cool gases.
  • Let’s look at some hot and cool gases in space.
slide13

Horsehead Nebula – copyright Arne Henden

Dust obscuring Ha emission nebula

slide14

Orion Nebula – copyright Robert Gendler

  • 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.
cold dark clouds
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.
gravity vs pressure
Gravity vs. Pressure
  • Stars and other interstellar material are in a perpetual battle between forces pushing 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.
star formation

COOLER

HOTTER

Star Formation
  • Remember lecture 2A:
  • Cold interstellar clouds:

No heat = no velocity = no outward pressure.

Gravity wins.

  • Gas begins to contract.
1 the interstellar cloud
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:
    • If a star’s worth of matter should clump together in a denser region than the rest of the cloud:
    • Gravitational attraction will win out over their combined pressure.
    • The clump will begin to collapse.
    • The cold cloud will fragment.
  • Time: A few million years.
2 contracting fragments
2. Contracting Fragments
  • A fragment about the same mass as the Sun slowly contracts due to its gravity.
  • Now a few hundredths of a parsec across or 100 times the size of the Solar System.
  • Temperature still about the same.
  • In the center some heat begins to be retained.
  • Time: several tens of thousands of years.
3 continued contraction
3. Continued Contraction
  • Fragment now a gaseous sphere.
  • Size of the Solar System
    • (10,000 x the size of the Sun)
  • Inner region is dense enough to be opaque to light (remember the convection zone of Sun).
    • Result: inner region heats up – 10,000 K.
    • Outer edge still cool.
  • The central opaque part is called a protostar.
  • Mass increases as material rains down on it.
  • Time: 100,000 years
4 protostellar evolution
4. Protostellar Evolution
  • Gravity is still winning.
  • The protostar is still shrinking.
  • Size: Mercury’s orbit.
  • The protostar is also still warming.
    • Core = 1,000,000 K (recall core of Sun 15,000,000 K)
    • Still not hot enough for nuclear fusion
    • Surface temp = 2000 – 3000 K (recall Sun = 5800 K)
the evolutionary track
The Evolutionary Track
  • Given the low temperature, the protostar has a low flux (very little energy is emitted per area of its surface).
  • The surface area is huge, however!
  • Result: Very high total luminosity (or absolute magnitude).
5 t tauri phase
5. T Tauri Phase
  • Protostar still shrinks: 10 x the Sun.
  • Smaller size  smaller surface area  smaller luminosity.
  • Luminosity = 10 x 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.
6 a star is born
6. A Star is Born
  • Time: 6 million years since the protostar formed (Stage 3).
  • 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 almost counter the contraction from gravity.
7 the main sequence
7. The Main Sequence
  • Time: 30 million years since Stage 6.
  • Central temp is finally 15,000,000 K
  • Pressure from energy of fusion balances gravity
    • Contraction ends
  • Surface temp is now 6000 K
  • 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.
now what
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
open clusters
Open Clusters
  • These are the new stars.
  • Small groups of young stars.
  • Slowly drifting apart.

Jewel Box – copyright MichaelBessell

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