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Title:
LWS Observations of Pre Main Sequence Objects
Authors:
Saraceno, P.; Nisini, B.; Benedettini, M.; Ceccarelli, C.; di Giorgio, A. M.; Giannini, T.; Molinari, S.; Spinogl, L.; Clegg, P. E.; Correia, J. C.; Griffin, M. J.; Leeks, S. J.; White, G. J.; Caux, E.; Lorenzetti, D.; Tommasi, E.; Liseau, R.; Smith, H. A.
Affiliation:
AA(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AB(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AC(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AD(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AE(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AF(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AG(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AH(Istituto di Fisica dello Spazio Interplanetario, CNR - Frascati, Italy), AI(Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK), AJ(Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK), AK(Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK), AL(Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK), AM(Queen Mary & Westfield College, Mile End Road, London E1 4NS, UK), AN(CESR, BP4346, F-31028 Toulouse Cedex O4, Franc), AO(Osservatorio di Roma, I-00040 Monteporzio, Italy), AP(ISO SOC, P.O.box 50727, 28080 Vilspa Spain), AQ(Stockholm Observatory, S-133 36 - Saltsjobaden, Sweden), AR(Smithsonian Center for Astrophysics, MA 02138 Cambridge, USA)
Publication:
Star Formation with the Infrared Space Observatory, 24-26 June 1997, Lisbon, Portugal, edited by Joao Yun and Rene Liseau, Publisher: ASP, as volume 132 of ASP Conference Series. P. 233.
Publication Date:
00/1998
Origin:
AUTHOR
Bibliographic Code:
1998ASPC..132..233S

Abstract

We review the first results of a 45-190 microns spectroscopic study of a sample of Class 0,~~Class I, ~~Class II (Herbig Ae/Be) and Herbig-Haro objects. In the observed Class 0, Class I and HH objects J shocks can account for the [OI] observed intensity, while for Ae/Be stars the [OI] emission is mainly due to the presence of photodissociation region. For some Class 0 and Class I sources, high-J CO transitions are the dominant FIR coolants, indicating the additional presence of C shocks. In these sources the H_2O cooling is significantly less than that predicted by models. Finally, evidence is seen for [OI] 63 microns self-absorption in all the Class I and the Class II objects of the sample.

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