Titlebook: Galactic Radio Astronomy; F. J. Kerr,S. C. Simonson Book 1974 International Astronomical Union 1974 Galaxy.astronomy.interstellar matter.p

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Galactic Radio Astronomy978-94-010-2263-7Series ISSN 1743-9213 Series E-ISSN 2352-2186

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https://doi.org/10.1007/978-1-4020-9500-9es, self-absorption features in emission profiles, and absorption profiles in the directions of discrete sources. It is concluded that the intercloud medium in the solar neighbourhood has a temperature between 10. and 10. K, a column density of ~1.4×10. cosec |.| atoms cm., and a brightness temperat

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The Snow Line in Red Dwarf Systems.Interstellar optical absorption lines and H. 21-cm emission lines show a number of very large aggregates with properties similar to those of ‘cloud complexes’. At nonzero velocities especially for . < 0°, exist optical lines which have no Hi counterparts. These are almost certainly produced in low-

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Spatial Query Broker in a Grid Environmenty means of computerized procedures. Maps of some of the clouds so defined are presented, and their properties discussed. Many clouds are elongated and/or irregular in shape. Histograms of cloud parameters are presented and subjected to statistical analysis. There is evidence for tenuous clouds of la

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Spina-Bifida

Short Note About Geophysical Data Analysis,in the visible, to more than 30. The distribution and properties of an important constituent of the interstellar gas, molecular hydrogen, can be studied in detail using this instrument. A more comprehensive picture may now be developed for element depletion factors, electron densities, and sources o

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Valerie Lindsay,Michel Rod,Nicholas Ashill that many of the pulsars observed have distances greater than 5 kpc, leading to an upper limit of about 0.03 cm. for the mean electron density. The electron density averaged over distances of a few hundred parsecs seems to be very constant. The width of the electron distribution in the .-direction

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