Universe: Stars And Galaxies
Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 18, Problem 4Q
To determine

(a)

The evidence that proves the presence of the interstellar gases.

To determine

(b)

The evidence that proves that there is dust in the interstellar medium.

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(a) Rank the following components of the interstellar medium in order of the wavelengths at which they are observed, longest wavelength first: clouds of neutral hydrogen, coronal gas, interstellar dust, nebulae. Longest to Shortest?   (b) Rank the same material in order of decreasing temperature from hottest to coolest. Hottest to Coolest?
Based on what you know about observations of the interstellar medium at wavelengths other than for visible light, select all of the correct statements from the following list. -The 21-cm radio observations are of neutral hydrogen. -Much interstellar dust between stars is not visible. -The source of hot gas observed at X-ray wavelengths is not known. -All interstellar material is cool. -Interstellar dust is observed at ultraviolet wavelengths. -Giant molecular clouds consist mostly of CO molecules. -Material observed at wavelengths longer than that of visible light is usually cool.
How are giant molecular clouds (GMCs), the loci of most star formation, themselves formed out of diffuse interstellar gas? What processes determine the distribution of physical conditions within star-forming regions, and why does star formation occur in only a small fraction of the available gas? How is the rate at which stars form determined by the properties of the natal GMC or, on a larger scale, of the interstellar medium (ISM) in a galaxy? What determines the mass distribution of forming stars, the initial mass function (IMF)? Most stars form in clusters (Lada & Lada 2003); how do stars form in such a dense environment and in the presence of enormous radiative and mechanical feedback from other YSOs?
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