Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...322..275m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 322, Nov. 1, 1987, p. 275-287. NASA-supported research.
Astronomy and Astrophysics
Astronomy
38
Molecular Clouds, Radio Astronomy, Shock Waves, Stellar Models, Stellar Winds, Bipolarity, Electron Density (Concentration), Radio Sources (Astronomy), Stellar Luminosity, Stellar Temperature
Scientific paper
Fast dissociative shocks in molecular clouds are shown to produce detectable radio recombination lines and continuum in addition to optical and infrared recombination lines. Impact broadening sets an upper limit to the brightness of radio recombination lines. Detailed numerical models of the shock structure are used to calculate the effective emission measure, the intensity of optically thin recombination lines, and the effective temperature of the emitting region for shocks with velocities between 40 and 150 km s-1 propagating in gas of density 104cm-3≤ n0≤ 106cm-3. The results are applied to shocks in bipolar flows from young stellar objects in molecular clouds. The H51α line observed by Hasegawa and Akabane in 1984 in Orion-KL is interpreted as emission from a shock in a stellar wind at a velocity of about 70 km s-1.
Hollenbach David J.
McKee Christopher F.
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