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Far-IR Spectrophotometry of HH Flows with the ISO Long-Wavelength Spectrometer

Published online by Cambridge University Press:  25 May 2016

R. Liseau ,
T. Giannini ,
B. Nisini ,
P. Saraceno ,
L. Spinoglio ,
B. Larsson ,
D. Lorenzetti  and
E. Tommasi
R. Liseau
Affiliation:
Stockholm Observatory, S-133 36 Saltsjöbaden, Sweden e-mail: [email protected]
T. Giannini
Affiliation:
CNR-Istituto di Fisica dello Spazio Interplanetario, I–000 44 Frascati, Italy
B. Nisini
Affiliation:
CNR-Istituto di Fisica dello Spazio Interplanetario, I–000 44 Frascati, Italy
P. Saraceno
Affiliation:
CNR-Istituto di Fisica dello Spazio Interplanetario, I–000 44 Frascati, Italy
L. Spinoglio
Affiliation:
CNR-Istituto di Fisica dello Spazio Interplanetario, I–000 44 Frascati, Italy
B. Larsson
Affiliation:
Stockholm Observatory, S-133 36 Saltsjöbaden, Sweden
D. Lorenzetti
Affiliation:
Osservatorio Astronomico di Roma, I–000 40 Monte Porzio, Italy
E. Tommasi
Affiliation:
Lws Instrument Dedicated Team, Iso Science Operations Centre Villafranca de Castillo, Spain

Abstract

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Full Iso-Lws spectral scans between about 45 to 190 μm of 17 individual HH objects in 7 star forming regions have revealed essentially only [O I] 63 μm line emission, implying that the Fircooling of these objects is totally dominated by this line alone. In this case, J-shock models can be used to determine the mass loss rates of the HH exciting sources. These mass loss rates are in reasonably good agreement with those estimated for the accompanying CO flows, providing first observational evidence that HH and molecular flows are driven by the same agent. The Lmech – Lbol relation, based on our results with the Lws, implies that young stellar objects of lower mass are loosing mass at relatively higher rates than their more massive counterparts.

Type
I. Herbig-Haro Objects, H2 Flows and Radio Jets
Information
Symposium - International Astronomical Union , Volume 182: Herbig-Haro Flows and the Birth of Low Mass Stars , 1997 , pp. 111 - 120
Copyright
Copyright © Kluwer 1997 

References

Bally, J., Lane, A.P., 1991, in: Lada, C.J. & Kylafis, N.D. (eds.) The physics of star formation and early stellar evolution, Kluwer, p. 471.Google Scholar
Cabrit, S., Bertout, C., 1992, A&A 261, 274.Google Scholar
Clegg, P.E. et al., 1996, A&A 315, L 38.Google Scholar
Cohen, M., Hollenbach, D.J., Haas, M.R., Erickson, E.F., 1988, ApJ 329, 863.Google Scholar
Draine, B.T., Roberge, W.G., Dalgarno, A., 1983, ApJ 264, 485.Google Scholar
Edwards, S., Ray, T., Mundt, R., 1993, in: Levy, E.H. & Lunine, J.I. (eds.), Protostars and Planets III, U. Arizona, p. 567.Google Scholar
Hartigan, P., Morse, J.A., Heathcote, S., Gerald, C., 1993, ApJ 414, L 121.Google Scholar
Hollenbach, D.J., 1985, Icarus 61, 36.Google Scholar
Hollenbach, D., McKee, C.F., 1989, ApJ 342, 306.Google Scholar
Hollenbach, D.J., Takahashi, T., Tielens, A.G.G.M., 1991, ApJ 377, 192.CrossRefGoogle Scholar
Kessler, M. et al., 1996, A&A 315, L 27.Google Scholar
Lada, C.J., 1985, ARA&A 23, 267.Google Scholar
Liseau, R. et al., 1996, A&A 315, L 181.Google Scholar
Nisini, B. et al., 1996, A&A 315, L 321.Google Scholar
Swinyard, B.M. et al., 1996, A&A 315, L 43.Google Scholar
Wolfire, M.G., Tielens, A.G.G.M., Hollenbach, D., 1990, ApJ 358, 116.Google Scholar