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hal.structure.identifierAMOR 2015
dc.contributor.authorREBOUSSIN, Laura
hal.structure.identifierAMOR 2015
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierAMOR 2015
dc.contributor.authorGUILLOTEAU, S.
hal.structure.identifierECLIPSE 2015
dc.contributor.authorHERSANT, F.
hal.structure.identifierAMOR 2015
dc.contributor.authorDUTREY, Anne
dc.date.issued2015
dc.identifier.issn0004-6361
dc.description.abstractEnThe gas mass of protoplanetary disks, and the gas-to-dust ratio, are two key elements driving the evolution of these disks and the formation of planetary system. We explore here to what extent CO (or its isotopologues) can be used as a tracer of gas mass. We use a detailed gas-grain chemical model and study the evolution of the disk composition, starting from a dense pre-stellar core composition. We explore a range of disk temperature profiles, cosmic rays ionization rates, and disk ages for a disk model representative of T Tauri stars. At the high densities that prevail in disks, we find that, due to fast reactions on grain surfaces, CO can be converted to less volatile forms (principally s-CO$_2$, and to a lesser extent s-CH$_4$) instead of being evaporated over a wide range of temperature. The canonical gas-phase abundance of 10$^{-4}$ is only reached above about 30-35 K. The dominant Carbon bearing entity depends on the temperature structure and age of the disk. The chemical evolution of CO is also sensitive to the cosmic rays ionization rate. Larger gas phase CO abundances are found in younger disks. Initial conditions, such as parent cloud age and density, have a limited impact. This study reveals that CO gas-phase abundance is heavily dependent on grain surface processes, which remain very incompletely understood so far. The strong dependence on dust temperature profile makes CO a poor tracer of the gas-phase content of disks.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Earth and Planetary Astrophysics
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.title.enChemistry in Protoplanetary Disks: the gas-phase CO/H2 ratio and the Carbon reservoir
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201525885
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1505.01309
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A82
bordeaux.volume579
bordeaux.peerReviewedoui
hal.identifierhal-01149639
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01149639v1
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