Volume 429, Number 2, January II 2005
|Page(s)||509 - 523|
|Section||Interstellar and circumstellar matter|
|Published online||17 December 2004|
A far UV study of interstellar gas towards HD 34078: High excitation H2 and small scale structure*
Institut d'Astrophysique de Paris, 75014 Paris, France
2 LERMA/ENS, France
3 LUTH, Observatoire de Paris-Meudon, 92195 Meudon Cedex, France
4 Onsala Space Observatory, 439 92 Onsala, Sweden
5 Institute of Astronomy, Cambridge, UK
6 IAS, Université d'Orsay, 91405 Orsay Cedex, France
7 Johns Hopkins University, Baltimore, USA
8 ESA, Vilspa, Spain
9 Laboratoire d'Astrophysique de Marseille, 13376 Marseille, France
10 LESIA, Observatoire de Paris-Meudon, 92195 Meudon Cedex, France
Accepted: 12 July 2004
To investigate the presence of small scale structure in the spatial distribution of H2 molecules we have undertaken repeated FUSE UV observations of the runaway O9.5V star, HD 34078. In this paper we present five spectra obtained between January 2000 and October 2002. These observations reveal an unexpectedly large amount of highly excited H2. Column densities for H2 levels from (, ) up to (, ) and for several and levels are determined. These results are interpreted in the frame of a model involving essentially two components: i) a foreground cloud (unaffected by HD 34078) responsible for the H2 (, 1), CI, CH, CH+ and CO absorptions; ii) a dense layer of gas ( cm-3) close to the O star and strongly illuminated by its UV flux which accounts for the presence of highly excited H2. Our model successfully reproduces the H2 excitation, the CI fine-structure level populations as well as the CH, CH+ and CO column densities. We also examine the time variability of H2 absorption lines tracing each of these two components. From the stability of the , 1 and 2 damped H2 profiles we infer a 3σ upper limit on column density variations (H2)/N(H2) of 5% over scales ranging from 5 to 50 AU. This result clearly rules out any pronounced ubiquitous small scale density structure of the kind apparently seen in HI. The lines from highly excited gas are also quite stable (equivalent to %) indicating i) that the ambient gas through which HD 34078 is moving is relatively uniform and ii) that the gas flow along the shocked layer is not subject to marked instabilities.
Key words: stars: individual: HD 34078 / ISM: structure / ISM: molecules / ISM: clouds
© ESO, 2005
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.