Small scale structure in molecular gas from multi-epoch observations of HD 34078

Details Small scale structure in molecular gas from multi-epoch observations of HD 34078 Small scale structure in molecular gas from multi-epoch observations of HD 34078

2003-01-23

arxiv.org/abs/astro-ph/0301474v2

Astron.Astrophys. 401 (2003) 215-226

Astronomy and Astrophysics

Astrophysics

12 pages, 14 figures. accepted for publication in A&A. v2 : the few notes on the absorption line at 5772 AA have been removed

Scientific paper

10.1051/0004-6361:20030103

We present spectroscopic observations of the runaway reddened star HD 34078 acquired during the last three years at Observatoire de Haute Provence and McDonald Observatory as well as other spectra obtained since 1990. The drift of the line of sight through the foreground cloud due to the large transverse velocity of HD 34078 allows us to probe the spatial distribution of CH, CH+, CN and DIBs carriers at scales ranging from about 1 AU up to 150 AU. In particular, time variations in the equivalent width of absorption lines are examined. A few past and recent high resolution observations of CH and CH+ absorption are used to search for line profile variations and to convert equivalent widths into column densities. The data set reveals a 20 % increase in CH column density over the past 10 years with no corresponding variation in the column density of CH+ or in the strengths of the 5780 and 5797 AA DIBs. CN observations indicate that its excitation temperature has significantly increased from < 3.1 K in 1993 to 3.6 +- 0.17 K in 1998 while the CN column shows only a modest rise of ~ 12 +- 6 %. The data also strongly suggest the existence of weak correlated variations in CH and CH+ columns over periods of 6 - 12 months (or ~ 10 AU). These results are discussed in relation to CH+ production mechanisms. A dense newly intervening clump is considered in order to explain the long-term increase in the column density of CH, but such a scenario does not account for all observational constraints. Instead, the observations are best described by CH+ production in a photodissociation region, like that suggested for the Pleiades and IC 348.

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