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

Liseau, R., Ceccarelli, C., Larsson, B., Nisini, B., White, G. J., Ade, Peter A. R. ORCID: https://orcid.org/0000-0002-5127-0401, Armand, C., Burgdorf, M., Caux, E., Cerulli, R., Church, S., Clegg, P. E., Digorgio, A., Furniss, I., Giannini, T., Glencross, W., Gry, C., King, K., Lim, T., Lorenzetti, D., Molinari, S., Naylor, D., Orfei, R., Saraceno, P., Sidher, S., Smith, H., Spinoglio, L., Swinyard, B., Texier, D., Tommasi, E., Trams, N. and Unger, S. 1996. Thermal H_2_O emission from the Herbig-Haro flow HH 54. Astronomy and Astrophysics 315 , pp. 181-184.

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Abstract

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.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	stars: formation, ism: molecules, ism: jets and outflows, ism: individual objects: hh 54, physical processes: shock waves, physical processes: radiative transfer
Publisher:	EDP Sciences
ISSN:	0004-6361
Last Modified:	28 Oct 2022 09:52
URI:	https://orca.cardiff.ac.uk/id/eprint/75933

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