Titlebook: CO: Twenty-Five Years of Millimeter-Wave Spectroscopy; Proceedings of the 1 William B. Latter,Simon J. E. Radford,John Bally Conference pro

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The Ursa Major Molecular Cloudsentered at (.) ∼ (138°,30°) and easily seen in IRAS 100 μm emission, is some 60 pc across and 150 pc distant (Meyerdierks et. al 1991). At 100 μm, the Ursa Major clouds appear in projection as “finger” (. ∼ 140,. ∼; 38) which “hangs down” towards the center of the loop and the plane of the Galaxy. D

GUILE

珍奇

The CO 2-1/1-0 Ratio solar neighborhood exhibit variations of the .=2−1/ .=l−0 intensity ratio from place to place in a cloud and from one cloud to another. This mainly reflects a variation of the hydrogen density near the ., where the opacity of the lines reaches ∼ 1 at cloud surfaces. The ratio often exceeds unity at

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Project

On the Fractal Structure of Molecular Cloudsects of star formation. Being generated predominantly by the turbulent internal cloud motion, the structure of molecular clouds is likely to be random to a large degree. As the information on the structural properties of random function is basically contained in its power spectrum, it is obviously i

grandiose

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偏离

冷峻

Narratives of Hurricane Katrina in Contextes easier to understand the evolution of the disk of stars. The star formation rate per unit molecular gas mass is constant as a function of radius, and the H. depletion time turns out to be only a few percent of the Hubble time. This very short timescale requires that the atomic gas act as a reserv

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https://doi.org/10.1007/978-3-319-59957-1a sensitivity per solid angle 3-10 times higher than previous CO surveys of the plane, and 16 times higher than the only previous extensive wide-latitude survey (Dame et al. 1987). Since a preliminary purpose of this survey is the study of molecular gas out of the plane in the inner Galaxy, the obse