2005A&A...429..509B

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 (v=0, J=0) up to (v=0, J=11) and for several v=1 and v=2 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 (J=0, 1), CI, CH, CH⁺ and CO absorptions; ii) a dense layer of gas (n≃10⁴cm^–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 J=0, 1 and 2 damped H₂ profiles we infer a 3σ upper limit on column density variations ΔN(H₂)/N(H₂) of 5% over scales ranging from 5 to 50AU. 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 ΔN/N≤30%) 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.