Other
Scientific paper
Jul 1966
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1966natur.211..503c&link_type=abstract
Nature, Volume 211, Issue 5048, pp. 503-504 (1966).
Other
63
Scientific paper
A MAJOR problem in the study of galactic radio emission from OH is to understand how it is that the emissions appear to be localized in very small bright regions each characterized by a particular frequency1; in addition, it has been found that emissions can show both linear and circular polarization2,3. The localization of emission at a particular frequency can readily be explained on the hypothesis of stimulated emission4 if there are regions in which the velocities of the OH molecules are correlated over large distances. Should the velocities vary considerably along a line of sight, so will the Doppler shifts relative to some local standard and stimulated emission will not occur because the optical depth at any particular frequency would be inadequate. For a sufficient optical depth, the velocities along the line of sight must be correlated over a distance of about 1019 cm. In the absence of shifts of wave-length from any other cause, the velocity must be constant along the line of sight over such a distance. Only in those directions along which there is such a systematic motion will intense emission be observed. The frequencies of peaks in observed spectra indicate that velocities in different parts of a source may differ by 100 km/s (ref. 1).
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