Star Formation

Learning Objectives

By the end of this section, you will be able to:

As we begin our exploration of how stars are formed, let’s review some basics about stars discussed in earlier chapters:

If we want to find stars still in the process of formation, we must look in places that have plenty of the raw material from which stars are assembled. Since stars are made of gas, we focus our attention (and our telescopes) on the dense and cold clouds of gas and dust that dot the Milky Way (see [link] and [link]).

Two Images of the Eagle Nebula (M16). Figure a shows the central region of the nebula, with two huge columns gas and dust silhouetted against the bright nebulosity in the background. Figure b shows a close-up of one of the columns of gas and dust. Along the bright portion of the top edge of the column, thin wisps of gas are seen radiating off and away from the pillar. This structure is known as an evaporating gas globule.

Molecular Clouds: Stellar Nurseries

As we saw in Between the Stars: Gas and Dust in Space, the most massive reservoirs of interstellar matter—and some of the most massive objects in the Milky Way Galaxy—are the giant molecular clouds. These clouds have cold interiors with characteristic temperatures of only 10–20 K; most of their gas atoms are bound into molecules. These clouds turn out to be the birthplaces of most stars in our Galaxy.

The masses of molecular clouds range from a thousand times the mass of the Sun to about 3 million solar masses. Molecular clouds have a complex filamentary structure, similar to cirrus clouds in Earth’s atmosphere, but much less dense. The molecular cloud filaments can be up to 1000 light-years long. Within the clouds are cold, dense regions with typical masses of 50 to 500 times the mass of the Sun; we give these regions the highly technical name clumps. Within these clumps, there are even denser, smaller regions called cores. The cores are the embryos of stars. The conditions in these cores—low temperature and high density—are just what is required to make stars. Remember that the essence of the life story of any star is the ongoing competition between two forces: gravity and pressure. The force of gravity, pulling inward, tries to make a star collapse. Internal pressure produced by the motions of the gas atoms, pushing outward, tries to force the star to expand. When a star is first forming, low temperature (and hence, low pressure) and high density (hence, greater gravitational attraction) both work to give gravity the advantage. In order to form a star—that is, a dense, hot ball of matter capable of starting nuclear reactions deep within—we need a typical core of interstellar atoms and molecules to shrink in radius and increase in density by a factor of nearly 1020. It is the force of gravity that produces this drastic collapse.

The Orion Molecular Cloud

Let’s discuss what happens in regions of star formation by considering a nearby site where stars are forming right now. One of the best-studied stellar nurseries is in the constellation of Orion, The Hunter, about 1500 light-years away ([link]). The pattern of the hunter is easy to recognize by the conspicuous “belt” of three stars that mark his waist. The Orion molecular cloud is much larger than the star pattern and is truly an impressive structure. In its long dimension, it stretches over a distance of about 100 light-years. The total quantity of molecular gas is about 200,000 times the mass of the Sun. Most of the cloud does not glow with visible light but betrays its presence by the radiation that the dusty gas gives off at infrared and radio wavelengths.

The Constellation of Orion in Visible and Infrared Light. In figure a, on the left, Orion is shown in visible light. The bright stars that define the figure, belt, and sword of the mythical hunter are connected with blue lines. Fainter stars pepper the background of this image. Figure b shows the same field in infrared light. Only cool stars, such as Betelgeuse, are visible. The image is dominated by extensive regions of bright yellow clumps, orange swirls, and red tendrils of gas and dust.

The stars in Orion’s belt are typically about 5 million years old, whereas the stars near the middle of the “sword” hanging from Orion’s belt are only 300,000 to 1 million years old. The region about halfway down the sword where star formation is still taking place is called the Orion Nebula. About 2200 young stars are found in this region, which is only slightly larger than a dozen light-years in diameter. The Orion Nebula also contains a tight cluster of stars called the Trapezium ([link]). The brightest Trapezium stars can be seen easily with a small telescope.

Close-up of the Orion Nebula in Infrared and Visible Light. Figure a, on the left, displays the nebula in infrared light. The image has few stars, and swirls of reddish nebulosity nearly cover the field of view. The Trapezium is seen as a bright patch near the center. Figure b shows the same region in visible light. Many more stars are seen, and the visible nebulosity is much smaller in extent. Pink and blue are the dominant colors of the nebula in visible light.

Compare this with our own solar neighborhood, where the typical spacing between stars is about 3 light-years. Only a small number of stars in the Orion cluster can be seen with visible light, but infrared images—which penetrate the dust better—detect the more than 2000 stars that are part of the group ([link]).

The Central Region of the Orion Nebula in visible and infrared light. Figure a, on the left, shows the Trapezium cluster of stars and the surrounding nebulosity. The four brightest stars of the Trapezium, plus a few others, are seen embedded in clouds of gas and dust. Figure b, on the right, shows the same field in infrared wavelengths. Many more stars are seen because infrared light penetrates the dust in the nebula.

Studies of Orion and other star-forming regions show that star formation is not a very efficient process. In the region of the Orion Nebula, about 1% of the material in the cloud has been turned into stars. That is why we still see a substantial amount of gas and dust near the Trapezium stars. The leftover material is eventually heated, either by the radiation and winds from the hot stars that form or by explosions of the most massive stars. (We will see in later chapters that the most massive stars go through their lives very quickly and end by exploding.)

Whether gently or explosively, the material in the neighborhood of the new stars is blown away into interstellar space. Older groups or clusters of stars can now be easily observed in visible light because they are no longer shrouded in dust and gas ([link]).

Image of Westerlund 2. Near the center of the image is the tight cluster of recently formed stars, with very little nebulosity surrounding them. Below and to the left is an arc-shaped region of nebulosity which extends out to near the edge of the image. The portion of the nebula nearest the star cluster is fairly smooth and featureless. The outer portions of the gas cloud farther from the cluster contains dark silhouetted pillars and globules, similar in appearance to those seen in the Eagle Nebula.

Although we do not know what initially caused stars to begin forming in Orion, there is good evidence that the first generation of stars triggered the formation of additional stars, which in turn led to the formation of still more stars ([link]).

Diagram of Propagating Star Formation. At left are depicted two old groups of stars. Below these groups a distance scale of 100 light years is shown. At the center of the diagram is a smaller, tighter grouping of young stars. To the right of the young group is an arc of compressed gas and an even tighter grouping of protostars within the arc. On the extreme right of the diagram adjacent to the protostars, a dark molecular cloud is portrayed.

The basic idea of triggered star formation is this: when a massive star is formed, it emits a large amount of ultraviolet radiation and ejects high-speed gas in the form of a stellar wind. This injection of energy heats the gas around the stars and causes it to expand. When massive stars exhaust their supply of fuel, they explode, and the energy of the explosion also heats the gas. The hot gases pile into the surrounding cold molecular cloud, compressing the material in it and increasing its density. If this increase in density is large enough, gravity will overcome pressure, and stars will begin to form in the compressed gas. Such a chain reaction—where the brightest and hottest stars of one area become the cause of star formation “next door”—seems to have occurred not only in Orion but also in many other molecular clouds.

There are many molecular clouds that form only (or mainly) low-mass stars. Because low-mass stars do not have strong winds and do not die by exploding, triggered star formation cannot occur in these clouds. There are also stars that form in relative isolation in small cores. Therefore, not all star formation is originally triggered by the death of massive stars. However, there are likely to be other possible triggers, such as spiral density waves and other processes we do not yet understand.

The Birth of a Star

Although regions such as Orion give us clues about how star formation begins, the subsequent stages are still shrouded in mystery (and a lot of dust). There is an enormous difference between the density of a molecular cloud core and the density of the youngest stars that can be detected. Direct observations of this collapse to higher density are nearly impossible for two reasons. First, the dust-shrouded interiors of molecular clouds where stellar births take place cannot be observed with visible light. Second, the timescale for the initial collapse—thousands of years—is very short, astronomically speaking. Since each star spends such a tiny fraction of its life in this stage, relatively few stars are going through the collapse process at any given time. Nevertheless, through a combination of theoretical calculations and the limited observations available, astronomers have pieced together a picture of what the earliest stages of stellar evolution are likely to be.

The first step in the process of creating stars is the formation of dense cores within a clump of gas and dust ([link](a)). It is generally thought that all the material for the star comes from the core, the larger structure surrounding the forming star. Eventually, the gravitational force of the infalling gas becomes strong enough to overwhelm the pressure exerted by the cold material that forms the dense cores. The material then undergoes a rapid collapse, and the density of the core increases greatly as a result. During the time a dense core is contracting to become a true star, but before the fusion of protons to produce helium begins, we call the object a protostar.

Illustration of the Formation of a Star. Part a, on the far left, shows a roughly spherical region containing many clumps of gas and dust. A scale is given to this region and is labeled 5000 AU. To the right is part b, showing one of these clumps as a sphere embedded in a faint disk of material. Arrows surround the sphere and disk, all pointing toward the center of the sphere, indicating inflow of material. Further to the right is part c, showing the same sphere and disk. Arrows are drawn pointing toward the disk to indicate inflow, and arrows perpendicular to the disk and pointing away from the poles of the sphere, indicating outflow of material. Finally, at far right, is part d, again showing a sphere embedded in a disk. No arrows are drawn. A scale is given for part d, and is labeled 100 AU.

The natural turbulence inside a clump tends to give any portion of it some initial spinning motion (even if it is very slow). As a result, each collapsing core is expected to spin. According to the law of conservation of angular momentum (discussed in the chapter on Orbits and Gravity), a rotating body spins more rapidly as it decreases in size. In other words, if the object can turn its material around a smaller circle, it can move that material more quickly—like a figure skater spinning more rapidly as she brings her arms in tight to her body. This is exactly what happens when a core contracts to form a protostar: as it shrinks, its rate of spin increases.

But all directions on a spinning sphere are not created equal. As the protostar rotates, it is much easier for material to fall right onto the poles (which spin most slowly) than onto the equator (where material moves around most rapidly). Therefore, gas and dust falling in toward the protostar’s equator are “held back” by the rotation and form a whirling extended disk around the equator (part b in [link]). You may have observed this same “equator effect” on the amusement park ride in which you stand with your back to a cylinder that is spun faster and faster. As you spin really fast, you are pushed against the wall so strongly that you cannot possibly fall toward the center of the cylinder. Gas can, however, fall onto the protostar easily from directions away from the star’s equator.

The protostar and disk at this stage are embedded in an envelope of dust and gas from which material is still falling onto the protostar. This dusty envelope blocks visible light, but infrared radiation can get through. As a result, in this phase of its evolution, the protostar itself is emitting infrared radiation and so is observable only in the infrared region of the spectrum. Once almost all of the available material has been accreted and the central protostar has reached nearly its final mass, it is given a special name: it is called a T Tauri star, named after one of the best studied and brightest members of this class of stars, which was discovered in the constellation of Taurus. (Astronomers have a tendency to name types of stars after the first example they discover or come to understand. It’s not an elegant system, but it works.) Only stars with masses less than or similar to the mass of the Sun become T Tauri stars. Massive stars do not go through this stage, although they do appear to follow the formation scenario illustrated in [link].

Winds and Jets

Recent observations suggest that T Tauri stars may actually be stars in a middle stage between protostars and hydrogen-fusing stars such as the Sun. High-resolution infrared images have revealed jets of material as well as stellar winds coming from some T Tauri stars, proof of interaction with their environment. A stellar wind consists mainly of protons (hydrogen nuclei) and electrons streaming away from the star at speeds of a few hundred kilometers per second (several hundred thousand miles per hour). When the wind first starts up, the disk of material around the star’s equator blocks the wind in its direction. Where the wind particles can escape most effectively is in the direction of the star’s poles.

Astronomers have actually seen evidence of these beams of particles shooting out in opposite directions from the popular regions of newly formed stars. In many cases, these beams point back to the location of a protostar that is still so completely shrouded in dust that we cannot yet see it ([link]).

Image of Gas Jets Flowing Away from HH 34. This figure presents three images of HH 34, taken in 1995, 1998, and 2000. The appearance of the jets that propagate away from the protostellar disk has changed in each image as clumps of material move outward along the length of the jet.

On occasion, the jets of high-speed particles streaming away from the protostar collide with a somewhat-denser lump of gas nearby, excite its atoms, and cause them to emit light. These glowing regions, each of which is known as a Herbig-Haro (HH) object after the two astronomers who first identified them, allow us to trace the progress of the jet to a distance of a light-year or more from the star that produced it. [link] shows two spectacular images of HH objects.

Outflows from Protostars. Two images of Herbig-Haro objects are presented. Figure a, at top, shows the HH 47, with an irregularly shaped jet emerging from the disk on the right-hand side of the image. On the left-hand side of the image, the jet eventually collides with interstellar gas producing a bow-shock. This has the appearance of an arrowhead, or an open umbrella. Figure b, on the bottom, shows HH 1 and HH 2. The jets are not visible, but at each end of the image the bow-shocks created by the jets crashing into the interstellar medium are seen.

The wind from a forming star will ultimately sweep away the material that remains in the obscuring envelope of dust and gas, leaving behind the naked disk and protostar, which can then be seen with visible light. We should note that at this point, the protostar itself is still contracting slowly and has not yet reached the main-sequence stage on the H–R diagram (a concept introduced in the chapter The Stars: A Celestial Census). The disk can be detected directly when observed at infrared wavelengths or when it is seen silhouetted against a bright background ([link]).

Disks around Protostars. This figure presents images of disks around the protostars CoKu Tau 1, DG Tau B, Haro 6-5B, IRAS 04016+2610, IRAS 04248+2612, and IRAS 04302+2247. A scale of 500 AU is shown on each image. The morphology is similar in each case: a butterfly-shaped nebula, crossed at the apex of the “wings” by a dark band of dust.

This description of a protostar surrounded by a rotating disk of gas and dust sounds very much like what happened in our solar system when the Sun and planets formed. Indeed, one of the most important discoveries from the study of star formation in the last decade of the twentieth century was that disks are an inevitable byproduct of the process of creating stars. The next questions that astronomers set out to answer was: will the disks around protostars also form planets? And if so, how often? We will return to these questions later in this chapter.

To keep things simple, we have described the formation of single stars. Many stars, however, are members of binary or triple systems, where several stars are born together. In this case, the stars form in nearly the same way. Widely separated binaries may each have their own disk; close binaries may share a single disk.

Key Concepts and Summary

Most stars form in giant molecular clouds with masses as large as 3 × 106 solar masses. The most well-studied molecular cloud is Orion, where star formation is currently taking place. Molecular clouds typically contain regions of higher density called clumps, which in turn contain several even-denser cores of gas and dust, each of which may become a star. A star can form inside a core if its density is high enough that gravity can overwhelm the internal pressure and cause the gas and dust to collapse. The accumulation of material halts when a protostar develops a strong stellar wind, leading to jets of material being observed coming from the star. These jets of material can collide with the material around the star and produce regions that emit light that are known as Herbig-Haro objects.

Glossary

giant molecular clouds
large, cold interstellar clouds with diameters of dozens of light-years and typical masses of 105 solar masses; found in the spiral arms of galaxies, these clouds are where stars form
Herbig-Haro (HH) object
luminous knots of gas in an area of star formation that are set to glow by jets of material from a protostar
protostar
a very young star still in the process of formation, before nuclear fusion begins
stellar wind
the outflow of gas, sometimes at speeds as high as hundreds of kilometers per second, from a star

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