Prediction of maser emission from para-H2O at 1.635 MM and 922 microns

Details Prediction of maser emission from para-H2O at 1.635 MM and 922 microns Prediction of maser emission from para-H2O at 1.635 MM and 922 microns

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...148..145c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 148, no. 1, July 1985, p. 145-150. DFG-supported research.

Astronomy and Astrophysics

Astrophysics

6

Interstellar Matter, Millimeter Waves, Molecular Collisions, Radiative Transfer, Water Masers, Cosmic Dust, Hydrogen, Molecular Energy Levels, Molecular Rotation, Optical Thickness, Stellar Evolution

Scientific paper

Non-LTE calculations have been performed for para-H2O. The coupled set of statistical and radiative transfer equations has been solved numerically in an on-the-spot approximation. The authors used a physical model in which the excitation is basically due to collisions. The results indicate that when the combined influence of resonant collisions with H2 molecules in the (J = 2)-state and absorption of IR-photons by cold dust are taken into account, fairly strong maser emission at 1.635 mm and 922 μ is to be expected from regions of star formation.

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