| dc.creator |
Cernicharo, José |
|
| dc.creator |
Goicoechea, Javier R. |
|
| dc.creator |
Daniel, Fabien |
|
| dc.creator |
Lerate, M. R. |
|
| dc.creator |
Barlow, Michael J. |
|
| dc.creator |
Swinyard, Bruce M. |
|
| dc.creator |
Dishoeck, E. van |
|
| dc.creator |
Lim, Tanya L. |
|
| dc.creator |
Viti, S. |
|
| dc.creator |
Yates, J. |
|
| dc.date |
2007-12-27T09:42:31Z |
|
| dc.date |
2007-12-27T09:42:31Z |
|
| dc.date |
2006-08-16 |
|
| dc.date.accessioned |
2017-01-31T00:59:32Z |
|
| dc.date.available |
2017-01-31T00:59:32Z |
|
| dc.identifier |
The Astrophysical Journal Letters, 649:L33–L36, 2006 September 20 |
|
| dc.identifier |
arXiv:astro-ph/0608336v1 |
|
| dc.identifier |
1538-4357 |
|
| dc.identifier |
http://hdl.handle.net/10261/2615 |
|
| dc.identifier |
10.1086/508259 |
|
| dc.identifier.uri |
http://dspace.mediu.edu.my:8181/xmlui/handle/10261/2615 |
|
| dc.description |
Accepted 2006 August 7; To be published in ApJ letters |
|
| dc.description |
We present the detection and modeling of more than 70 far-IR pure rotational lines of water vapor, including the 18O and 17O isotopologues, towards Orion KL. Observations were performed with the Long Wavelength Spectrometer Fabry-Perot (LWS/FP; R~6800-9700) on board the Infrared Space Observatory (ISO) between ~43 and ~197 μm. The water line profiles evolve from P-Cygni type profiles (even for the H2O18 lines) to pure emission at wavelengths above ~100 μm. We find that most of the water emission/absorption arises from an extended flow of gas expanding at 25+-5 kms^-1. Non-local radiative transfer models show that much of the water excitation and line profile formation is driven by the dust continuum emission. The derived beam averaged water abundance is 2-3x10^-5. The inferred gas temperature Tk=80-100 K suggests that: (i) water could have been formed in the "plateau" by gas phase neutral-neutral reactions with activation barriers if the gas was previously heated (e.g. by shocks) to >500 K and/or (ii) H2O formation in the outflow is dominated by in-situ evaporation of grain water-ice mantles and/or (iii) H2O was formed in the innermost and warmer regions (e.g. the hot core) and was swept up in ~1000 yr, the dynamical timescale of the outflow. |
|
| dc.description |
Peer reviewed |
|
| dc.format |
924446 bytes |
|
| dc.format |
application/pdf |
|
| dc.language |
eng |
|
| dc.relation |
Preprint |
|
| dc.rights |
openAccess |
|
| dc.subject |
Astrophysics |
|
| dc.subject |
ISM: lines and bands |
|
| dc.subject |
ISM: individual (Orion) |
|
| dc.subject |
ISM: molecule |
|
| dc.subject |
Line:identification |
|
| dc.subject |
Radiative transfer |
|
| dc.title |
The Water Vapor Abundance in Orion KL Outflows |
|
| dc.type |
Pre-print |
|