Afficher la notice abrégée

Evolutionary view through the starless cores in Taurus

dc.contributor.authorNAVARRO-ALMAIDA, D.
dc.contributor.authorFUENTE, A.
dc.contributor.authorMAJUMDAR, L.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorWAKELAM, V.
dc.contributor.authorCASELLI, P.
dc.contributor.authorRIVIÈRE-MARICHALAR, P.
dc.contributor.authorTREVIÑO-MORALES, S.
dc.contributor.authorCAZAUX, S.
dc.contributor.authorJIMÉNEZ-SERRA, I.
dc.contributor.authorKRAMER, C.
dc.contributor.authorCHACÓN-TANARRO, A.
dc.contributor.authorKIRK, J.
dc.contributor.authorWARD-THOMPSON, D.
dc.contributor.authorTAFALLA, M.
dc.date.issued2021-09
dc.identifier.issn0004-6361
dc.description.abstractEnContext. The chemical and physical evolution of starless and pre-stellar cores are of paramount importance to understanding the process of star formation. The Taurus Molecular Cloud cores TMC 1-C and TMC 1-CP share similar initial conditions and provide an excellent opportunity to understand the evolution of the pre-stellar core phase. Aims. We investigated the evolutionary stage of starless cores based on observations towards the prototypical dark cores TMC 1-C and TMC 1-CP. Methods. We mapped the prototypical dark cores TMC 1-C and TMC 1-CP in the CS 3 → 2, C 34 S 3 → 2, 13 CS 2 → 1, DCN 1 → 0, DCN 2 → 1, DNC 1 → 0, DNC 2 → 1, DN 13 C 1 → 0, DN 13 C 2 → 1, N 2 H + 1 → 0, and N 2 D + 1 → 0 transitions. We performed a multi-transitional study of CS and its isotopologs, DCN, and DNC lines to characterize the physical and chemical properties of these cores. We studied their chemistry using the state-of-the-art gas-grain chemical code N AUTILUS and pseudo time-dependent models to determine their evolutionary stage. Results. The central n H volume density, the N 2 H + column density, and the abundances of deuterated species are higher in TMC 1-C than in TMC 1-CP, yielding a higher N 2 H + deuterium fraction in TMC 1-C, thus indicating a later evolutionary stage for TMC 1-C. The chemical modeling with pseudo time-dependent models and their radiative transfer are in agreement with this statement, allowing us to estimate a collapse timescale of ~1 Myr for TMC 1-C. Models with a younger collapse scenario or a collapse slowed down by a magnetic support are found to more closely reproduce the observations towards TMC 1-CP. Conclusions. Observational diagnostics seem to indicate that TMC 1-C is in a later evolutionary stage than TMC 1-CP, with a chemical age ~1 Myr. TMC 1-C shows signs of being an evolved core at the onset of star formation, while TMC 1-CP appears to be in an earlier evolutionary stage due to a more recent formation or, alternatively, a collapse slowed down by a magnetic support.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enEvolutionary view through the starless cores in Taurus
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202140820
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv2107.00423
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA15
bordeaux.volume653
bordeaux.peerReviewedoui
hal.identifierhal-03795691
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03795691v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2021-09&rft.volume=653&rft.spage=A15&rft.epage=A15&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=NAVARRO-ALMAIDA,%20D.&FUENTE,%20A.&MAJUMDAR,%20L.&WAKELAM,%20V.&CASELLI,%20P.&rft.genre=article


Fichier(s) constituant ce document

FichiersTailleFormatVue

Il n'y a pas de fichiers associés à ce document.

Ce document figure dans la(les) collection(s) suivante(s)

Afficher la notice abrégée