Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.207..339s&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 207, March 15, 1984, p. 339-354.
Astronomy and Astrophysics
Astrophysics
78
Astronomical Models, Interstellar Masers, Optical Pumping, Radiant Flux Density, Water Masers, Protoplanets, Stellar Envelopes, Stellar Evolution, Stellar Mass, Stellar Winds
Scientific paper
It is shown that the minimum pump power necessary to explain the observed energy flux in a maser line is proportional to 1/l-cubed, where l is the amplification length. The probable upper limits for l are estimated from the observed velocity gradients in several H2O clusters associated with the regions of star formation: they vary from about 0.5 to about 50 AU. Using the 'equivalent pumping transition' approximation, it is argued that with such small l all the previous models fail to explain the observed maser energy fluxes. It is shown that the degree of ionization in the H2O condensations could be much higher than commonly believed, and that the electrons could be there appreciably cooler than the H2 molecules. Two possible astrophysical models, based on the collision-collisional pump working in such a two-temperature gas, are proposed. It is suggested that the origin of the maser condensations can be related with the formation of giant protoplanets.
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