Afficher la notice abrégée

hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONNE, Lars
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierPhysikalisches Institut [Köln]
dc.contributor.authorSCHNEIDER, Nicola
hal.structure.identifierPhysikalisches Institut [Köln]
dc.contributor.authorCLARKE, Seamus
hal.structure.identifierInstituto de Astrofísica e Ciências do Espaço [IASTRO]
dc.contributor.authorARZOUMANIAN, Doris
hal.structure.identifierDepartment of Physics [Nagoya]
dc.contributor.authorFUKUI, Yasuo
hal.structure.identifierDepartment of Physics [Nagoya]
dc.contributor.authorTACHIHARA, Kengo
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCSENGERI, Timea
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorGUESTEN, Rolf
hal.structure.identifierDepartment of Physics [Nagoya]
dc.contributor.authorOHAMA, Akio
hal.structure.identifierDepartment of Physics [Nagoya]
dc.contributor.authorOKAMOTO, R
hal.structure.identifierPhysikalisches Institut [Köln]
dc.contributor.authorSIMON, R
hal.structure.identifierGeometry and Statistics in acquisition data [GeoStat]
dc.contributor.authorYAHIA, Hussein
hal.structure.identifierDepartment of Physics [Nagoya]
dc.contributor.authorYAMAMOTO, Hiroaki
dc.date.created2020-10-19
dc.date.issued2020-10-19
dc.identifier.issn0004-6361
dc.description.abstractEnDense molecular filaments are ubiquituous in the interstellar medium, yet their internal physical conditions and the role of gravity, turbulence, the magnetic field, radiation and the ambient cloud during their evolution remain debated. Aims. We study the kinematics and physical conditions in the Musca filament, the ambient cloud and the Chamaeleon-Musca complex, to constrain the physics of filament formation. Methods. We produce CO(2-1) isotopologue maps with APEX that cut through the Musca filament. We further study a NANTEN2 12 CO(1-0) map of the full Musca cloud, H I emission of the Chamaeleon-Musca complex, a Planck polarisation map, line radiative tranfer models, GAIA data and synthetic observations from filament formation simulations. Results. The Musca cloud, with a size of ∼ 3-6 pc, contains multiple velocity components. Radiative transfer modelling of the CO emission indicates that the Musca filament consists of a cold (∼10 K), dense (n H 2 ∼10 4 cm −3) crest, best described with a cylindrical geometry. Connected with the crest, a separate gas component at T∼15 K and n H 2 ∼10 3 cm −3 is found, the so-called strands. The velocity-coherent filament crest has an organised transverse velocity gradient that is linked to the kinematics of the nearby ambient cloud. This velocity gradient has an angle ≥ 30 • with respect to the local magnetic field orientation derived from Planck, and the magnitude of the velocity gradient is similar to the transonic linewidth of the filament crest. Studying the large scale kinematics, we find coherence of the asymmetric kinematics from the 50 pc H I cloud down to the Musca filament. We also report a strong [C 18 O]/[ 13 CO] abundance drop by an order of magnitude from the filament crest to the strands over a distance < 0.2 pc in a weak ambient FUV-field. Conclusions. The dense Musca filament crest is a long-lived (several crossing times) dynamic structure that can form stars in the near future because of continuous mass accretion replenishing the filament. This mass accretion on the filament appears to be triggered by a H I cloud-cloud collision which bends the magnetic field around dense filaments. This bending of the magnetic field is then responsible for the observed asymmetric accretion scenario of the Musca filament, which is for instance seen as a V-shape in the PV diagram.
dc.description.sponsorshipGENeration et Evolution des Structures du milieu InterStellaire - ANR-16-CE92-0035
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enISM: structure
dc.title.enFormation of the Musca filament: evidence for asymmetries in the accretion flow due to a cloud-cloud collision
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202038281
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.peerReviewedoui
hal.identifierhal-02967378
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02967378v1
bordeaux.COinSctx_ver=Z39.88-2004&amp;rft_val_fmt=info:ofi/fmt:kev:mtx:journal&amp;rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&amp;rft.date=2020-10-19&amp;rft.eissn=0004-6361&amp;rft.issn=0004-6361&amp;rft.au=BONNE,%20Lars&amp;BONTEMPS,%20Sylvain&amp;SCHNEIDER,%20Nicola&amp;CLARKE,%20Seamus&amp;ARZOUMANIAN,%20Doris&amp;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