Astronomy 162: Professor Barbara Ryden

Wednesday, January 22

STAR FORMATION


``Then there was a star danced, and under that was I born.''
- William Shakespeare, Much Ado About Nothing, 2, 1

Key Concepts


(1) Stars form when dense clumps of interstellar gas collapse gravitationally.

Consider a small, dense dark nebula (also known as a `Bok globule'). The luminosity of the dense core, using the equation which relates luminosity to radius and temperature, is:
L = 170 Lsun.
Thus, the dense core is over 100 times more luminous than the star it is destined to become! However, since T = 10K, the wavelength of maximum emission is:
Lambdamax = 0.29 millimeters (in the far infrared, which is hard to detect from the Earth's surface).

To convert a dense core into a star, we must both compress it (decreasing R by a factor of 4,400,000) and heat it (increasing T by a factor of 580).

Dense interstellar clouds are ordinarily stable. To start their collapse, we must first compress them with a shock wave traveling through the interstellar medium. One source of shock waves is supernovas (exploding stars).

Above is an image (taken with the Hubble Space Telescope) of a supernova shock wave, in the constellation Cygnus, slamming into a molecular cloud. The colors are computer-enhanced; the interstellar medium isn't really as gaudy as this picture. Click on the image to see an enlarged, higher-resolution version.
(Image credit: Jeff Hester [Arizona State University], and NASA)


(2) The collapsing gas heats up and becomes a PROTOSTAR

After the initial trigger provided by the passing shock wave, the inward force of gravity is greater than the outward pressure force. The gas cloud starts to collapse, and becomes a protostar. As the center of the protostar is compressed, it heats up. However, the protostar is initially very opaque, and the heat at the center of the protostar takes a long time to reach the surface. Thus, during the initial stages of the protostar's collapse, its surface temperature T is constant, while its radius R decreases; as a consequence, the luminosity L decreases. Eventually, the heat from the center of the protostar makes its way to the surface. When this happens, the surface temperature T and the luminosity L both increase, while the radius R remains almost constant.

The protostar is not in isolation; it is surrounded by a rotating accretion disk in the equatorial plane, and a bipolar outflow at its north and south poles.

The disk is important because it is capable of fragmenting into planets (the planets around the Sun are thought to have formed in this way).
The outflow is important because it sweeps away the excess gas and dust in the vicinity of the protostar.

Above are two images (taken 11 months apart, using the Hubble Space Telescope) of the disk and bipolar outflow associated with a protostar named HH30. The outflow is aligned horizontally; the disk (which is divided in two by a dust lane down its middle) is aligned vertically. Click on the image to see an enlarged higher-resolution version.
(Image credit: C. Burrows [Space Telescope Science Institute], and NASA)


Note: if the protostar is rotating too rapidly, it becomes unstable, and breaks apart into two protostars orbiting each other. Thus, binary systems are thought to originate from dense cores which are rotating more rapidly.

(3) A protostar stops collapsing when nuclear fusion begins in its center

The protostar is still collapsing inward, although far more slowly now. It is becoming smaller and hotter. What stops it from collapsing until it becomes a black hole?

The center of the protostar, which is becoming hotter and denser with time, eventually reaches the point where it is so hot and so dense, hydrogen nuclei start to fuse together to form helium nuclei. At this point, the protostar has a fusion reactor at its center, and is now called a star. When four H nuclei fuse to form helium, energy is released. The energy raises the temperature and the pressure inside the star.

We have now reached the stable situation where the outward force of pressure is sufficient to balance the inward force of gravity. The star stops collapsing, and starts its sedate life as a main sequence star, which lasts as long as the hydrogen holds out.

Protostars less massive than 0.08 Msun never become hot enough for fusion to start; they become brown dwarfs.

Protostars more massive than 200 Msun literally blow themselves apart before they can become stars. Such massive protostars are very luminous. The bright light they emit pushes on the outer layers of the protostar (just as sunlight pushes on a comet's tail). The outward force due to starlight is greater than the inward force of gravity, and the star is blown away, starting with the outer layer and working inward.


Prof. Barbara Ryden (ryden@astronomy.ohio-state.edu)

Updated: 2003 Jan 22

Copyright 2003, Barbara Ryden