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Molecular evolution in star-forming cores: From prestellar cores to protostellar cores

hal.structure.identifierDepartment of Earth and Planetary Sciences [Kobe]
dc.contributor.authorAIKAWA, Yuri
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierInstitut de biologie et chimie des protéines [Lyon] [IBCP]
dc.contributor.authorSAKAI, Nami
hal.structure.identifierDepartment of Physics, The Ohio State University
dc.contributor.authorGARROD, R. T.
hal.structure.identifierDepartment of Physics [OHIO STATE UNIVERSITY]
dc.contributor.authorHERBST, E.
dc.contributor.authorYAMAMOTO, Satoshi
dc.date.issued2008
dc.date.conference2008
dc.description.abstractEnWe investigate the molecular abundances in protostellar cores by solving the gas-grain chemical reaction network. As a physical model of the core, we adopt a result of one-dimensional radiation-hydrodynamics calculation, which follows the contraction of an initially hydrostatic prestellar core to form a protostellar core. Temporal variation of molecular abundances is solved in multiple infalling shells, which enable us to investigate the spatial distribution of molecules in the evolving core. The shells pass through the warm region of T ~ 20 100 K in several 104 yr and falls onto the central star in ~100 yr after they enter the region of T > 100 K. We found that the complex organic species such as HCOOCH3 are formed mainly via grain-surface reactions at T ~ 20 40 K, and then sublimated to the gas phase when the shell temperature reaches their sublimation temperatures (T ≥ 100 K). Carbon-chain species can be re-generated from sublimated CH4 via gas-phase and grain-surface reactions. HCO2+, which is recently detected towards L1527, are abundant at r = 100 2,000 AU, and its column density reaches ~1011 cm‑2 in our model. If a core is isolated and irradiated directly by interstellar UV radiation, photo-dissociation of water ice produces OH, which reacts with CO to form CO2 efficiently. Complex species then become less abundant compared with the case of embedded core in ambient clouds. Although a circumstellar (protoplanetary) disk is not included in our core model, we can expect similar chemical reactions (i.e., production of large organic species, carbon-chains and HCO2+) to proceed in disk regions with T ~ 20 100 K.
dc.language.isoen
dc.source.title2008IAUS..251..129A - Organic Matter in Space, Proceedings of the International Astronomical Union, IAU Symposium
dc.subject.enStars: formation
dc.subject.enISM: molecules
dc.typeCommunication dans un congrès
dc.identifier.doi10.1017/S1743921308021364
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]/Planétologie et astrophysique de la terre [astro-ph.EP]
bordeaux.page129-136
bordeaux.volume251
bordeaux.countryFR
bordeaux.title.proceeding2008IAUS..251..129A - Organic Matter in Space, Proceedings of the International Astronomical Union, IAU Symposium
bordeaux.peerReviewedoui
hal.identifierhal-00403449
hal.version1
hal.invitednon
hal.proceedingsoui
hal.popularnon
hal.audienceInternationale
dc.title.itMolecular evolution in star-forming cores: From prestellar cores to protostellar cores
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00403449v1
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