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| DC Field | Value | Language |
|---|---|---|
| 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 | - |
| Appears in Collections: | Digital Csic | |
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