Mostrar el registro sencillo del ítem

Compression and ablation of the photo-irradiated cloud the Orion Bar

hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorGOICOECHEA, Javier R.,
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
dc.contributor.authorPETY, J.,
dc.contributor.authorCUADRADO, S.,
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorCERNICHARO, J.,
hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierAMOR 2016
dc.contributor.authorCHAPILLON, E.
dc.contributor.authorFUENTE, A.,
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorGERIN, M.,
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
dc.contributor.authorJOBLIN, C.,
hal.structure.identifierIstituto di Radioastronomia [Bologna] [IRA]
dc.contributor.authorMARCELINO, N.,
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
dc.contributor.authorPILLERI, P.,
dc.date.issued2016-08
dc.identifier.issn0028-0836
dc.description.abstractEnThe Orion Bar is the archetypal edge-on molecular cloud surface illuminated by strong ultraviolet radiation from nearby massive stars. Owing to the close distance to Orion (about 1,350 light-year), the effects of stellar feedback on the parental cloud can be studied in detail. Visible-light observations of the Bar(1) show that the transition between the hot ionised gas and the warm neutral atomic gas (the ionisation front) is spatially well separated from the transition from atomic to molecular gas (the dissociation front): about 15 arcseconds or 6,200 astronomical units (one astronomical unit is the Earth-Sun distance). Static equilibrium models(2,3) used to interpret previous far-infrared and radio observations of the neutral gas in the Bar(4,5,6) (typically at 10-20 arcsecond resolution) predict an inhomogeneous cloud structure consisting of dense clumps embedded in a lower density extended gas component. Here we report one-arcsecond-resolution millimetre-wave images that allow us to resolve the molecular cloud surface. In contrast to stationary model predictions(7,8,9), there is no appreciable offset between the peak of the H2 vibrational emission (delineating the H/H2 transition) and the edge of the observed CO and HCO+ emission. This implies that the H/H2 and C+/C/CO transition zones are very close. These observations reveal a fragmented ridge of high-density substructures, photoablative gas flows and instabilities at the molecular cloud surface. The results suggest that the cloud edge has been compressed by a high-pressure wave that currently moves into the molecular cloud. The images demonstrate that dynamical and nonequilibrium effects are important for the cloud evolution.
dc.language.isoen
dc.publisherNature Publishing Group
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enCompression and ablation of the photo-irradiated cloud the Orion Bar
dc.typeArticle de revue
dc.identifier.doi10.1038/nature18957
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1608.06173
bordeaux.journalNature
bordeaux.page207-209
bordeaux.volume537
bordeaux.issue7619
bordeaux.peerReviewedoui
hal.identifierhal-01357743
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01357743v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Nature&rft.date=2016-08&rft.volume=537&rft.issue=7619&rft.spage=207-209&rft.epage=207-209&rft.eissn=0028-0836&rft.issn=0028-0836&rft.au=GOICOECHEA,%20Javier%20R.,&PETY,%20J.,&CUADRADO,%20S.,&CERNICHARO,%20J.,&CHAPILLON,%20E.&rft.genre=article


Archivos en el ítem

ArchivosTamañoFormatoVer

No hay archivos asociados a este ítem.

Este ítem aparece en la(s) siguiente(s) colección(ones)

Mostrar el registro sencillo del ítem