Ceccarelli, C.; Caux, E.; White, G. J.; Molinari, S.; Furniss, I.; Liseau, R.; Nisini, B.; Saraceno, P.; Spinoglio, L. and Wolfire, M.
PDF (Version of Record)
- Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
|Google Scholar:||Look up in Google Scholar|
We report ISO-LWS observations toward the low mass star IRAS16293-2422 between 43µm - 197µm. The CO, H2O and OH rotational lines and the OI(63µm) fine-structure line dominate the spectrum. Combining the CO Jup=14 to 25 observations with previous Jup=6 measurements, we derive stringent limits on the density (~3 · 104cm-3), temperature (~1500 K), and column density (~1.5 · 1020cm-2) of the emitting gas. We show that this warm gas is associated with the outflow and that a low velocity, C-type shock can account for the characteristics of the CO spectrum. The H2O and OH abundances derived from the observed line fluxes are [H2O] / [H2] ~2 · 10-5 and [OH] / [H2] ~5 · 10-6 respectively. Finally, we speculate that the OI(63µm) line emission originates in the collapsing envelope that surrounds the central object.
|Item Type:||Conference Item|
|Copyright Holders:||1997 Astronomical Society of the Pacific|
|Extra Information:||Star Formation with the Infrared Space Observatory
ASP Conference Series, Vol.132, 1998
J. L. Yun, and R. Liseau, eds.
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||16 Mar 2012 09:43|
|Last Modified:||04 Oct 2016 17:16|
|Share this page:|
Download history for this item
These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.