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From Prestellar to Protostellar Cores. II. Time Dependence and Deuterium Fractionation
| dc.contributor.author | AIKAWA, Y. | |
| hal.structure.identifier | AMOR 2012 | |
| dc.contributor.author | WAKELAM, Valentine | |
| hal.structure.identifier | FORMATION STELLAIRE 2012 | |
| dc.contributor.author | HERSANT, F. | |
| hal.structure.identifier | The Ohio State University [Columbus] [OSU] | |
| dc.contributor.author | GARROD, R. T. | |
| hal.structure.identifier | Department of Physics [Ohio State University] [OSU] | |
| hal.structure.identifier | Ohio State Univ, Dept Astron & Chem, Columbus, OH 43210 USA | |
| dc.contributor.author | HERBST, E. | |
| dc.date.created | 2012-10-15 | |
| dc.date.issued | 2012-11 | |
| dc.identifier.issn | 0004-637X | |
| dc.description.abstractEn | We investigate the molecular evolution and D/H abundance ratios that develop as star formation proceeds from a dense molecular cloud core to a protostellar core, by solving a gas-grain reaction network applied to a one-dimensional radiative hydrodynamic model with infalling fluid parcels. Spatial distributions of gas and ice-mantle species are calculated at the first-core stage, and at times after the birth of a protostar. Gas-phase methanol and methane are more abundant than CO at radii r <~ 100 AU in the first-core stage, but gradually decrease with time, while abundances of larger organic species increase. The warm-up phase, when complex organic molecules are efficiently formed, is longer-lived for those fluid parcels infalling at later stages. The formation of unsaturated carbon chains (warm carbon-chain chemistry) is also more effective in later stages; C+, which reacts with CH4 to form carbon chains, increases in abundance as the envelope density decreases. The large organic molecules and carbon chains are strongly deuterated, mainly due to high D/H ratios in the parent molecules, determined in the cold phase. We also extend our model to simulate simply the chemistry in circumstellar disks, by suspending the one-dimensional infall of a fluid parcel at constant disk radii. The species CH3OCH3 and HCOOCH3 increase in abundance in 104-105 yr at the fixed warm temperature; both also have high D/H ratios. | |
| dc.language.iso | en | |
| dc.publisher | American Astronomical Society | |
| dc.subject.en | ISM: abundances | |
| dc.subject.en | ISM: clouds | |
| dc.subject.en | stars: formation | |
| dc.type | Article de revue | |
| dc.identifier.doi | 10.1088/0004-637X/760/1/40 | |
| dc.subject.hal | Planète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO] | |
| dc.subject.hal | Physique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO] | |
| dc.identifier.arxiv | 1210.2476 | |
| bordeaux.journal | The Astrophysical Journal | |
| bordeaux.page | 40 | |
| bordeaux.volume | 760 | |
| bordeaux.peerReviewed | oui | |
| hal.identifier | hal-00764165 | |
| hal.version | 1 | |
| hal.popular | non | |
| hal.audience | Internationale | |
| dc.title.it | From Prestellar to Protostellar Cores. II. Time Dependence and Deuterium Fractionation | |
| hal.origin.link | https://hal.archives-ouvertes.fr//hal-00764165v1 | |
| bordeaux.COinS | ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The%20Astrophysical%20Journal&rft.date=2012-11&rft.volume=760&rft.spage=40&rft.epage=40&rft.eissn=0004-637X&rft.issn=0004-637X&rft.au=AIKAWA,%20Y.&WAKELAM,%20Valentine&HERSANT,%20F.&GARROD,%20R.%20T.&HERBST,%20E.&rft.genre=article |
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