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Chapter 18: Problem 6

What are stationary absorption lines? In what sort of spectra are they seen? How do they give evidence for the existence of the interstellar medium?

Short Answer

Expert verified
Stationary absorption lines are spectral lines that don't shift regardless of the source's radial velocity. They're seen in absorption spectra, formed when light from a hot object passes through a cooler gas. They provide evidence for the existence of the Interstellar Medium (ISM) as they reveal its composition, temperature, and density when light from distant stars passes through the ISM, causing certain wavelengths to get absorbed and forming these lines.

Step by step solution

01

Understanding Stationary Absorption Lines

Stationary absorption lines are spectral lines in an astronomical spectrograph that remain in the same place regardless of the radial velocity (speed along the line of sight) of the source. These lines are formed when light passes through cooler gas and certain frequencies of light are absorbed by atoms or molecules in the gas.
02

Identifying In which Type of Spectra Are Stationary Absorption Lines Seen

Stationary absorption lines are generally seen in absorption spectra. An absorption spectrum is formed when light from a hot, dense object passes through a cooler gas. Because each element absorbs light at its unique set of frequencies, the absorption spectrum can help identify those elements.
03

Relating Absorption Lines to the Interstellar Medium

Stationary absorption lines provide evidence for the existence of the interstellar medium (ISM). The ISM is the matter and radiation that exists in the space between the star systems in a galaxy. As light from distant stars passes through the ISM, certain wavelengths of light are absorbed, creating the absorption lines we see in spectra. These absorption lines, in turn, reveal the composition, temperature, and density of the ISM.

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Most popular questions from this chapter

Find the density (in atoms per cubic centimeter) of a Bok globule having a radius of 1 light-year and a mass of \(100 \mathrm{M}_{\odot}\). How does your result compare with the density of a typical H II region, between 80 and 600 atoms per \(\mathrm{cm}^{3}\) ? (Assume that the globule is made purely of hydrogen atoms.)

Search the World Wide Web for recent discoveries about how brown dwarfs form. Do they tend to form in the same locations as "real" stars? Do they form in relatively small or relatively large numbers compared to "real" stars? What techniques are used to make these discoveries?

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If you looked at the spectrum of a reflection nebula, would you see absorption lines, emission lines, or no lines? Explain your answer. As part of your explanation, describe how the spectrum demonstrates that the light was reflected from nearby stars.

What sets the limits on the maximum and minimum masses of a main-sequence star?
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