Water line emission in low-mass protostars

Details Water line emission in low-mass protostars Water line emission in low-mass protostars

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..647c&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 647

Physics

Molecular Lines, Star Formation, Young Sources

Scientific paper

Using the Long Wavelength Spectrometer on board ISO, we have detected far infrared rotational H2O emission lines in five low-mass young stellar objects in a survey of seven such sources. The total H2O fluxes are well correlated with the 1.3 mm continuum fluxes, but - surprisingly - not with the SiO millimeter emission originating in the outflows, suggesting that the water emission arises either in the circumstellar envelopes or in slow and dense shocks in the outflows. In this contribution we analyze in detail the case of NGC1333-IRAS4 and IRAS16293-2422, in which we measured several H2O lines, and use their fluxes to put stringent constraints on the physical conditions (temperature, density and column density) of the emitting gas. Simple LVG modelling implies that the emission originates in a very small (~ 200 AU), dense (>= 107 cm-3) and warm (~ 100 K) region, with a column density larger than about 1016 cm-2. The detected H2O emission may be well accounted for by thermal emission from a collapsing envelope, and we derive constraints on the accretion rate and central mass of NGC1333-IRAS4. We also discuss an alternative scenario in which the H2O emission arises in an extremely dense shock very close to the central object, perhaps caused by the interaction of the outflow with the inner regions of the circumstellar envelope.

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