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Title:
Shock excited far-infrared molecular emission around T Tau
Authors:
Spinoglio, L.; Giannini, T.; Nisini, B.; van den Ancker, M. E.; Caux, E.; Di Giorgio, A. M.; Lorenzetti, D.; Palla, F.; Pezzuto, S.; Saraceno, P.; Smith, H. A.; White, G. J.
Affiliation:
AA(Istituto di Fisica dello Spazio Interplanetario, CNR, via Fosso del Cavaliere 100, 00133 Roma, Italy), AB(Istituto di Fisica dello Spazio Interplanetario, CNR, via Fosso del Cavaliere 100, 00133 Roma, Italy; Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio, Italy; Istituto Astronomico, UniversitàLa Sapienza, via Lancisi 29, 00161 Roma, Italy), AC(Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio, Italy), AD(Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands), AE(CESR, B.P. 4346, 31028 Toulouse Cedex 04, France), AF(Istituto di Fisica dello Spazio Interplanetario, CNR, via Fosso del Cavaliere 100, 00133 Roma, Italy), AG(Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monte Porzio, Italy), AH(Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy), AI(Istituto di Fisica dello Spazio Interplanetario, CNR, via Fosso del Cavaliere 100, 00133 Roma, Italy), AJ(Istituto di Fisica dello Spazio Interplanetario, CNR, via Fosso del Cavaliere 100, 00133 Roma, Italy), AK(Harvard - Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA, USA), AL(Physics Department, Queen Mary & Westfield College, University of London, Mile End Road, London E1 4NS, UK; Stockholm Observatory, 133 36 Saltsjobaden, Sweden)
Publication:
Astronomy and Astrophysics, v.353, p.1055-1064 (2000) (A&A Homepage)
Publication Date:
01/2000
Origin:
A&A
Astronomy Keywords:
INFRARED: ISM: LINES AND BANDS, ISM: JETS AND OUTFLOWS, ISM: INDIVIDUAL OBJECTS: T TAU, STARS: PRE-MAIN SEQUENCE, STARS: INDIVIDUAL: T TAU, STARS: FORMATION
Bibliographic Code:
2000A&A...353.1055S

Abstract

The first complete far-infrared spectrum of T Tau has been obtained with the LWS spectrometer on-board the Infrared Space Observatory (ISO), which detected strong emission from high-J (J=14-25) CO, para- and ortho-H_2O and OH transitions over the wavelength range from 40 to 190 mu m. In addition the [OI]63mu m, [OI]145mu m and [CII]158mu m atomic lines were also detected. Most of the observed molecular emission can be explained by a single emission region at T ~ 300-900 K and n_H_2 ~ 105-6cm-3, with a diameter of about 2-3 arcsec. This corresponds to a very compact region of 300 - 400 AU at the distance of 140 pc. A higher temperature component seems to be needed to explain the highest excitation CO and H_2O lines. We derive a water abundance of 1-7 * 10-5 and an OH abundance of ~ 3* 10-5 with respect to molecular hydrogen, implying H_2O and OH enhancements by more than a factor of 10 with respect to the expected ambient gas abundance. The observed cooling in the various species amounts to 0.04 Lsun, comparable to the mechanical luminosity of the outflow, indicating that the stellar winds could be responsible of the line excitation through shocks. In order to explain the observed molecular cooling in T Tau in terms of C-type shock models, we hypothesise that the strong far-ultraviolet radiation field photodissociates water in favour of OH. This would explain the large overabundance of OH observed. The estimated relatively high density and compactness of the observed emission suggest that it originates from the shocks taking place at the base of the molecular outflow emission, in the region where the action of the stellar winds from the two stars of the binary system is important. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) with the participation of ISAS and NASA

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