18.3 Dark Dust Clouds
Emission nebulae are only one small component of interstellar space. Most of spacein fact, more than 90 percent of itis devoid of nebular regions or superheated bubbles, and contains no stars. It is simply dark. Look again at Figure 18.5, or just ponder the evening sky. The dark regions are by far the most representative of interstellar space. The average temperature of a typical dark region of interstellar matter is about 100 K. Compare this with 273 K, at which water freezes, and 0 K, at which atomic and molecular motions cease. (More Precisely 3-1) Interstellar space is very cold.
Within these dark voids among the nebulae and the stars lurks another type of astronomical objectthe dark dust cloud. These clouds are even colder than their surroundings (with temperatures as low as a few tens of kelvins), and thousands or even millions of times denser. Along any given line of sight, their densities can range from 107 atoms/m3 to more than 1012 atoms/m3 (106 atoms/cm3). These latter clouds are generally called dense interstellar clouds by researchers, but even these densest interstellar regions are about as tenuous as the best laboratory vacuum. Still, it is because their density is much larger than the average value of 106 atoms/m3 that we can distinguish clouds from the surrounding expanse of interstellar space.
These clouds bear little resemblance to terrestrial clouds. Most are bigger than our solar system, and some are many parsecs across. (Yet even so, they make up no more than a few percent of the entire volume of interstellar space.) Despite their name, these clouds are made up primarily of gas, just like the rest of the interstellar medium. However, their absorption of starlight is due almost entirely to the dust they contain.
OBSCURATION OF VISIBLE LIGHT
Figures 18.12(a) and (b) are optical photographs of a typical interstellar dust cloud. Pockets of intense blackness mark regions where the dust and gas are especially concentrated and the light from background stars is completely obscured. This cloud takes its name from a nearby star, Rho Ophiuchi, and resides relatively nearbyabout 300 pc away. Measuring several parsecs across, this cloud is only a tiny part of the grand mosaic shown in Figure 18.5. This cloud clearly is far from spherical. Indeed, most interstellar clouds are very irregularly shaped. Note especially the long streamers of (relatively) dense dust and gas in Figure 18.12(b).
The bright patches within the dark region in Figure 18.12(a) are foreground objectsemission nebulae and groups of bright stars. Some of them are part of the cloud itself, where newly formed stars near the surface have created a hot spot in the cold, dark gas. Others have no connection to the cloud and just happen to lie along our line of sight. The additional foreground stars in Figure 18.12(b) are too faint to be seen on Figure 18.12(a).
Like all dark dust clouds, the Rho Ophiuchi cloud is too cold to emit any visible light. However, it does radiate strongly at longer wavelengths. Figure 18.12(c) shows an infrared view of the same region, captured by sensitive detectors aboard the Infrared Astronomy Satellite. (Sec. 5.6) These dark and dusty interstellar clouds are sprinkled throughout our Galaxy. We can study them at optical wavelengths only if they happen to block the light emitted by more distant stars or nebulae. The dark outline of Rho Ophiuchi in Figure 18.12(a) and the dust lanes visible in Figures 18.8, 18.9, and 18.12(b) are good examples of this obscuration. The dust is apparent because it blocks the light coming from behind it. Figure 18.13 shows another striking example of a dark cloudthe Horsehead Nebula in Orion. This curiously shaped finger of gas and dust projects out from the much larger dark cloud in the bottom half of the image and stands out clearly against the red glow of a background emission nebula.
Astronomers first became aware of the true extent of dark interstellar clouds in the 1930s as they studied the optical spectra of distant stars. The gas in the cloud absorbs some of the stellar radiation in a manner that depends on the clouds own temperature, density, and elemental abundance. The absorption lines thus produced contain information about dark interstellar matter, just as stellar absorption lines reveal the properties of stars. (Sec. 4.2) Because the interstellar absorption lines are produced by cold, low-density gas, astronomers can easily distinguish them from the much broader absorption lines formed in the stars hot lower atmospheres. (Sec. 4.4) Figure 18.14(a) illustrates how light from a star may pass through several interstellar clouds on its way to Earth. These clouds need not be close to the star, and indeed they usually are not. Each absorbs some of the stellar radiation in a manner that depends on its own temperature, density, velocity, and elemental abundance. Figure 18.14(b) depicts part of a typical spectrum produced in this way.
Figure 18.15 is a classic example of a dark cloud. Emitting no visible light, the region L977 in the constellation Cygnus is made up of cold gas which is mostly molecular in composition. Invisible to the eye except by the degree to which starlight is dimmed by the cloud, the clouds molecular emissionin this case in radiation from carbon monoxide (CO) molecules (see Section 18.5)outlines it clearly at radio wavelengths.
The narrow absorption lines contain information about dark interstellar clouds, just as stellar absorption lines reveal the properties of stars, and nebular emission lines tell us about conditions in hot nebulae. By studying these lines, astronomers can probe the cold depths of interstellar space. In most cases the elemental abundances detected in interstellar clouds mirror those found in other astronomical objectsperhaps not surprising, since interstellar clouds are the regions that spawn emission nebulae and stars.