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CH in absorption in IRAS16293-2422

hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorBOTTINELLI, S.
hal.structure.identifierAMOR 2014
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorCAUX, E.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorVASTEL, C.
dc.contributor.authorAIKAWA, Y.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorCECCARELLI, C.
dc.date.created2014-05-05
dc.date.issued2014
dc.identifier.issn0035-8711
dc.description.abstractEnWhile recent studies of the solar-mass protostar IRAS16293-2422 have focused on its inner arcsecond, the wealth of Herschel/HIFI data has shown that the structure of the outer envelope and of the transition region to the more diffuse ISM is not clearly constrained. We use rotational ground-state transitions of CH (methylidyne), as a tracer of the lower-density envelope. Assuming LTE, we perform a $\chi^2$ minimization of the high spectral resolution HIFI observations of the CH transitions at ~532 and ~536 GHz in order to derive column densities in the envelope and in the foreground cloud. We obtain column densities of (7.7$\pm$0.2)$\times10^{13}$ cm$^{-2}$ and (1.5$\pm$0.3)$\times10^{13}$ cm$^{-2}$, respectively. The chemical modeling predicts column densities of (0.5-2)$\times10^{13}$ cm$^{-2}$ in the envelope (depending on the cosmic-ray ionization rate), and 5$\times10^{11}$ to 2.5$\times10^{14}$ cm$^{-2}$ in the foreground cloud (depending on time). Both observed abundances are reproduced by the model at a satisfactory level. The constraints set by these observations on the physical conditions in the foreground cloud are however weak. Furthermore, the CH abundance in the envelope is strongly affected by the rate coefficient of the reaction H+CH$\rightarrow$C+H$_2$ ; further investigation of its value at low temperature would be necessary to facilitate the comparison between the model and the observations.
dc.language.isoen
dc.publisherOxford University Press (OUP): Policy P - Oxford Open Option A
dc.subject.enSolar and Stellar Astrophysics
dc.subject.enAstrophysics
dc.subject.enAstrophysics of Galaxies
dc.title.enCH in absorption in IRAS16293-2422
dc.typeArticle de revue
dc.identifier.doi10.1093/mnras/stu700
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1405.0846
bordeaux.journalMonthly Notices of the Royal Astronomical Society
bordeaux.page1964-1973
bordeaux.volume441
bordeaux.issue3
bordeaux.peerReviewedoui
hal.identifierhal-00988052
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00988052v1
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