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• W1159152383 endingPage "436" @default.
• W1159152383 startingPage "383" @default.
• W1159152383 abstract "This chapter focuses on the microwave transitions of interstellar atoms and molecules. Several hundred radio frequency (rf) spectrum lines have been detected in radiation from interstellar matter, most of them in emission but some also in absorption. There are three quantities used commonly for describing the intrinsic strength of a spectrum line, the transition probability A, the oscillator strength f, and the line strength S. Another useful parameter of the transition is the natural linewidth. Interstellar hyperfine transitions are detected from any excited electronic states of atomic hydrogen. In H I regions, where temperatures are low, virtually all the hydrogen atoms present are in n = 1. At higher temperatures where a reasonable fraction of the neutral atoms present is in n = 2, most atoms are ionized, so the excited state populations are still low. There are very few atomic fine-structure transitions at microwave frequencies; most of the transitions are in the infrared. Radio recombination lines are emitted after an electron has recombined with a positive ion. They are transitions in which the electron jumps among states with neighboring high values of the principal quantum number n (similar lines with low n are observed in the optical spectrum). They are seen in emission from hot interstellar regions (H II regions) where the atoms are predominantly ionized." @default.
• W1159152383 created "2016-06-24" @default.
• W1159152383 creator A5034498865 @default.
• W1159152383 date "1978-01-01" @default.
• W1159152383 modified "2023-09-26" @default.
• W1159152383 title "Microwave Transitions of Interstellar Atoms and Molecules" @default.
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