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Infrared Spectra of Stars

AND HISTOR CA SKETCH I L longer than 9000 A (0.9 p.). I nfrared studies of the Sun will be considered for their own sake but will frequently be called upon to help interpret the spectra of other stars. Infrared s tel lar photom e tr y will be discussed only when it can be used to study spectral features. Finally, our concern wiII be the stellar spectra, rather than the problems and triumphs of wavel ength s not instrumental technique. According to the terminology now in fairl y general use, the infrared is divided into This review of infr·ared spectroscopy will be restricted to stars, and to the following four regions: the near infrared, roughly 0 . 7-0.9 po, invisible to the eye but accessible to the N-type photographic emulsion; the one-micron region, roughly 0.9- 1 . 1 p., accessible to the Z emu lsion and to S 1 photocathodes; the two-micron region, rou ghly 1.2-2.5 J.L , in which PbS photocondu ctive cells are often used (hence sometimes called the "lead sulfide region") i and the far infrared, extending from about 3 p. to millimeter wavelengths and the domain of radio astronomy. These regions are quite http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Annual Review of Astronomy and Astrophysics Annual Reviews
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