Mostrar el registro sencillo del ítem

Water in Protoplanetary Disks: Deuteration and Turbulent Mixing

dc.contributor.authorFURUYA, Kenji
hal.structure.identifierDepartment of Earth and Planetary Sciences [Kobe]
dc.contributor.authorAIKAWA, Yuri
dc.contributor.authorNOMURA, Hideko
hal.structure.identifierFORMATION STELLAIRE 2013
dc.contributor.authorHERSANT, F.
hal.structure.identifierAMOR 2013
dc.contributor.authorWAKELAM, Valentine
dc.date.created2013-10-12
dc.date.issued2013
dc.identifier.issn0004-637X
dc.description.abstractEnWe investigate water and deuterated water chemistry in turbulent protoplanetary disks. Chemical rate equations are solved with the diffusion term, mimicking turbulent mixing in vertical direction. Water near the midplane is transported to the disk atmosphere by turbulence and destroyed by photoreactions to produce atomic oxygen, while the atomic oxygen is transported to the midplane and reforms water and/or other molecules. We find that this cycle significantly decreases column densities of water ice at r < 30 AU, where dust temperatures are too high to reform water ice effectively. The radial extent of such region depends on the desorption energy of atomic hydrogen. Our model indicates that water ice could be deficient even outside the sublimation radius. Outside this radius, the cycle decreases the D/H ratio of water ice from 2x10^-2, which is set by the collapsing core model, to 10^-4-10^-2 in 10^6 yr, without significantly decreasing the water ice column density. The resultant D/H ratios depend on the strength of mixing and the radial distance from the central star. Our finding suggests that the D/H ratio of cometary water (10^-3-10^-4) could be established (i.e. cometary water could be formed) in the solar nebula, even if the D/H ratio of water ice delivered to the disk was very high (10^-2).
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.title.enWater in Protoplanetary Disks: Deuteration and Turbulent Mixing
dc.typeArticle de revue
dc.identifier.doi10.1088/0004-637X/779/1/11
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Planétologie et astrophysique de la terre [astro-ph.EP]
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.arxiv1310.3342
bordeaux.journalThe Astrophysical Journal
bordeaux.pageid. 11
bordeaux.volume779
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-00874486
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00874486v1
bordeaux.COinSctx_ver=Z39.88-2004&amp;rft_val_fmt=info:ofi/fmt:kev:mtx:journal&amp;rft.jtitle=The%20Astrophysical%20Journal&amp;rft.date=2013&amp;rft.volume=779&amp;rft.issue=1&amp;rft.spage=id.%2011&amp;rft.epage=id.%2011&amp;rft.eissn=0004-637X&amp;rft.issn=0004-637X&amp;rft.au=FURUYA,%20Kenji&amp;AIKAWA,%20Yuri&amp;NOMURA,%20Hideko&amp;HERSANT,%20F.&amp;WAKELAM,%20Valentine&amp;rft.genre=article


Archivos en el ítem

ArchivosTamañoFormatoVer

No hay archivos asociados a este ítem.

Este ítem aparece en la(s) siguiente(s) colección(ones)

Mostrar el registro sencillo del ítem