Thermal H_2_O emission from the Herbig-Haro flow HH 54.

Details Thermal H_2_O emission from the Herbig-Haro flow HH 54. Thermal H_2_O emission from the Herbig-Haro flow HH 54.

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...315l.181l&link_type=abstract

Astronomy and Astrophysics, v.315, p.L181-L184

Astronomy and Astrophysics

Astrophysics

77

Stars: Formation, Ism: Molecules, Ism: Jets And Outflows, Ism: Individual Objects: Hh 54, Physical Processes: Shock Waves, Physical Processes: Radiative Transfer

Scientific paper

The first detection of thermal water emission from a Herbig-Haro object is presented. The observations were performed with the Lws (Long Wavelength Spectrograph) aboard Iso (Infrared Space Observatory). Besides H_2_O, rotational lines of CO are present in the spectrum of HH 54. These high-J CO lines are used to derive the physical model parameters of the Fir (far-infrared) molecular line emitting regions. This model fits simultaneously the observed OH and H_2_O spectra for an OH abundance X(OH)=10^-6^ and a water vapour abundance X(H_2_O)=10^-5^. At a distance of 250pc, the total CO, OH and H_2_O rotational line cooling rate is estimated to be 1.3x10^-2^Lsun_, which is comparable to the mechanical luminosity generated by the 10km/s shocks, suggesting that practically all of the cooling of the weak-shock regions is done by these three molecular species alone.

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