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The interstellar chemistry of C3H and C3H2 isomers

hal.structure.identifierInstitut des Sciences Moléculaires [ISM]
dc.contributor.authorLOISON, Jean-Christophe
hal.structure.identifierDepartamento de Engenharia Informática / Department of Informatics Engineering [DEI]
dc.contributor.authorMARCELINO, Marcelino
hal.structure.identifierAMOR 2017
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorROUEFF, Evelyne
hal.structure.identifierAMOR 2017
dc.contributor.authorGRATIER, P.
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorMARCELINO, Núria
hal.structure.identifierInstitut des Sciences Moléculaires [ISM]
dc.contributor.authorREYES, Dianailys Nuñez
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorCERNICHARO, José
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorGERIN, Maryvonne
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorAGÚNDEZ, Marcelino
dc.date.issued2017-10
dc.identifier.issn0035-8711
dc.description.abstractEnWe report the detection of linear and cyclic isomers of C3H and C3H2 towards various starless cores and review the corresponding chemical pathways involving neutral (C3Hx with x = 1,2) and ionic (C3Hx+ with x = 1,2,3) isomers. We highlight the role of the branching ratio of electronic dissociative recombination (DR) reactions of C3H2+ and C3H3+ isomers, showing that the statistical treatment of the relaxation of C3H* and C3H2* produced in these DR reactions may explain the relative c,l-C3H and c,l-C3H2 abundances. We have also introduced in the model the third isomer of C3H2 (HCCCH). The observed cyclic-to-linear C3H2 ratio varies from 110 ± 30 for molecular clouds with a total density of about 1 × 104 molecules cm-3 to 30 ± 10 for molecular clouds with a total density of about 4 × 105 molecules cm-3, a trend well reproduced with our updated model. The higher ratio for molecular clouds with low densities is determined mainly by the importance of the H + l-C3H2 → H + c-C3H2 and H + t-C3H2 → H + c-C3H2 isomerization reactions.
dc.language.isoen
dc.publisherOxford University Press (OUP): Policy P - Oxford Open Option A
dc.subject.enastrochemistry
dc.subject.enISM: abundances
dc.subject.enISM: clouds
dc.subject.enISM: molecules
dc.title.enThe interstellar chemistry of C3H and C3H2 isomers
dc.typeArticle de revue
dc.identifier.doi10.1093/mnras/stx1265
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1707.07926
bordeaux.journalMonthly Notices of the Royal Astronomical Society
bordeaux.page4075 - 4088
bordeaux.volume470
bordeaux.issue4
bordeaux.peerReviewedoui
hal.identifierhal-01583213
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01583213v1
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