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Astron. Astrophys. 331, 1070-1077 (1998)


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High velocity gas and dust evolution in Chamaeleon clouds *

Cecile Gry 1, François Boulanger 2, Edith Falgarone 3, Guillaume Pineau des Forêts 4 and James Lequeux 5

1 Laboratoire d'Astronomie Spatiale, B.P. 8, F-13376 Marseille cedex 12, France
2 Institut d'Astrophysique Spatiale Université Paris Sud, Bâtiment 121, F-91405 Orsay, France
3 Radioastronomie Millimétrique, Ecole Normale Supérieure, 24 Rue Lhomond, F-75005 Paris, France
4 DAEC, Observatoire de Paris, F-92195 Meudon Principal, France
5 Observatoire de Paris, 61 Avenue de l'Observatoire, F-75014 Paris, France

Received 6 September 1996 / Accepted 7 October 1997

Abstract

We report on GHRS observations which reveal conspicuous differences in the absorption spectra of two nearby stars, close to each other. The star HD102065 lies behind a cloud in Chamaeleon with unusually strong mid-IR emission, indicating a large abundance of very small dust particles. Along this line of sight, 5% of the gas (about 6 1019 cm-2) is at large velocities (up to -50 km s-1) compared to the main absorption component at [FORMULA] 0 km s-1. The high velocity gas is very excited and has an unusually large silicon abundance. The other star HD96675 lies behind a cloud with standard mid-IR emission. Along this line of sight, high velocity gas is also detected, but to somewhat smaller offset velocities and with a much lower excitation. In particular, the [FORMULA] lines are not observed.

From the excitation of [FORMULA] and [FORMULA] in the direction of HD102065, we infer that the high velocity gas has a temperature higher than several 100 K and an electron density of at least [FORMULA]. These results, together with the lack of an ionizing star in the neigborhood, suggest that a large amount of kinetic energy is being deposited in this gas. The collision of an infalling cloud and a local cloud is a plausible source of energy. The peculiarity of the dust size distribution inferred from the IRAS data is likely to be related to the processes which dissipate the kinetic energy and heat the gas. A shock seems to be required to produce the excitation and ionization degrees. But the carbon ionization ratio combined with the electron density inferred from the silicon and carbon excitation implies that carbon is not in ionization equilibrium and should recombine extremely quickly. Future higher resolution observations might help solving this incoherency.

Key words: ISM: Chamaeleon clouds – stars: HD 96675; HD 102065 – ISM: atoms; kinematics and dynamics – shocks

* Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.

© European Southern Observatory (ESO) 1998

Online publication: March 3, 1998
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