Star Formation Shapes the Appearance of the Universe and Provides the Sites for Planets

The Star Formation Process "We had the sky, up there, all speckled with stars, and we used to lay on our backs and look up at them, and discuss about whether they was made, or only just happened." - Mark Twain, Huckleberry Finn

Key points: How star formation starts; role of gravity; circumstellar disks; upper and lower mass limits for stars

Stars form in the centers of dense molecular cloudslink to an extra topic.

Generally speaking, we think most star formation proceeds along the same lines:

Step 1: initial collapse of an interstellar cloud

  • If the cloud can cool sufficiently, gravity will always cause a contraction and subsequent collapse. Many star-forming clouds appear to have collapsed spontaneously in this way.
  • As shown to the right, shock waves from supernovae explosions can hit a molecular cloud and compress it, causing parts to start collapsing under gravity into stars.(animation by G. Rieke)
  • The rotation of the Milky Way can cause clouds to pile up and collisions between clouds can cause their collapse under gravity (to be discussed when we get to galaxies).
inducedsf.gif (237584 bytes)

Step 2:  the cloud fragments into clumps that form individual stars buttonbook.jpg (10323 bytes). The fragmentation is related to turbulence in the collapsing cloud. (from Matthew Bate, http://www.astro.ex.ac.uk/people/mbate/Research/pr.html)

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A typical interstellar cloud is supported against collapse by internal turbulent motions. Once such a cloud is "tipped over the edge" and starts to collapse, it reaches a state where gravity can pull the gas together to form dense "cores". These cores continue to collapse, often fragmenting further, until they form star  - sized clumps.

Step 3: The clumps collapse into a stars

bate13.gif (29779 bytes) Once the force of gravity becomes larger than the pressure supporting the clumps, their collapse happens very fast.

Eventually the gas gets sufficiently compressed that it is dense and hot enough that the pressure balances the gravitational force, and the collapse stops. This situation is similar to the hydrostatic equilibrium we discussed for the sun. We call these objects "protostars."

This image of the massive star forming region RWC 49 shows a real-life ending to step 3 above. Stars have formed in the core of a molecular cloud and they have blown a hole in the cloud. You can see them glowing blue inside the hole. The remains of the cloud are heated by the new stars and glow pink. The image was obtained with the IRAC instrument on Spitzer, and ranges from 3.6 microns (blue) to 8 microns (red). Because it is an infrared image, we can see through the foreground dust that blocks our view in the visible region. (from Spitzer Science Center, http://www.spitzer.caltech.edu/Media/mediaimages/data.shtml)

 

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From protostar to main sequence:

Because the cloud core that collapses into a star is spinning, even slowly, when it gets down to star size it rotates rapidly - like an ice skater who starts a slow spin with her arms extended, and then accelerates when she brings them over her head. This rotation supports the gas around the equator of the new star as a disk, but the rest of the cloud falls directly into the star. Later, the star ejects some of the leftover material. As this disk spins, it creates a magnetic field that confines this material to a narrow jet. Drawing of a protostar/disk.jet system

 

These pictures show some examples of these disks and jets (illustrations and animation from STScI)
Protostars with surrounding disks and emerging jets animaiton show motion along protostellar jet
Here is an animation of a theoretical model of a protostellar jet like the one from HH47 above. The material in the jet cools rapidly, causing it to break up into clumps and "bullets". (From Jim Stone, http://www.astro.princeton.edu/~jstone/pjets.html)

 

Bowshock in material being ejected by young star After its initial collapse, the protostar is also likely still to be surrounded by a remnant of the cloud from which it formed.
  • eventually the star completes its contraction to the main sequence, where it begins to burn hydrogen, meanwhile blowing away this surrounding material. This HST image shows material ejected by the star in the center colliding with more quiescent nearby interstellar gas.
  • It is then observed as a normal main sequence star.

Fly through the Orion Nebula again and watch for some of these stages of star formation! en00500_1.jpg (18578 bytes)

Here is a summary (From TheEssential Cosmic Perspective, by Bennett et al.) Summary of process of stelalr formation, on the H-R diagram
On our HR diagram, the young stars heat up at nearly constant luminosity until they joint the main sequence (for example, the curve labeled 1.0 M).

Cloud clumps with .08 M < M < 100 M can form stable, main sequence stars.

hrprems.gif (64680 bytes)

What happens if the collapsing cloud is too small?

If the cloud has M < .08 M, it will contract, heat up, but the central temperature will never reach the 10,000,000oK limit required to start the conversion of H to He. The outer layers get warm, enough to appear similar to cool, dim stars for a few million years, but after that they steadily fade away. Such objects are called brown dwarfs. See the tracks on the HR diagram above labeled 0.01 M and 0.001 M.

What happens if the collapsing cloud is too large?

If the mass of the cloud exceeds about 100 M, it will collapse and heat up very quickly. Nuclear reactions occur so rapidly that the star becomes very luminous and blows itself apart -- either catastrophically or more gently by blowing off only the outer layers.

Consequences of star formation

Star formation "makes the Universe go 'round." In the following pages, we discuss some of the reasons.

Test your understanding before going onbuttongrad.jpg (11232 bytes)

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Marvel Quasar Comic, http://www.coincidental.net/comics/series/quasar/1-033.html

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Ultraviolet view of M81 enhances spiral arms, from APOD, NASA, UIT: http://antwrp.gsfc.nasa.gov/apod/ap960713.html

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hypertext copyright.jpg (1684 bytes) G. H. Rieke

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