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Autordc.contributor.authorEvans, Neal J.
Autordc.contributor.authorHeyer, Mark
Autordc.contributor.authorMiville Deschenes, Marc Antoine
Autordc.contributor.authorNguyen Luong, Quang
Autordc.contributor.authorMerello, Manuel
Fecha ingresodc.date.accessioned2022-03-03T20:06:19Z
Fecha disponibledc.date.available2022-03-03T20:06:19Z
Fecha de publicacióndc.date.issued2021
Cita de ítemdc.identifier.citationThe Astrophysical Journal, 920:126 (20pp), 2021 October 20es_ES
Identificadordc.identifier.other10.3847/1538-4357/ac1425
Identificadordc.identifier.urihttps://repositorio.uchile.cl/handle/2250/184015
Resumendc.description.abstractWe analyze surveys of molecular cloud structures defined by tracers ranging from CO J = 1 → 0 through 13CO J = 1 → 0 to dust emission together with NH3 data. The mean value of the virial parameter and the fraction of mass in bound structures depends on the method used to identify structures. Generally, the virial parameter decreases and the fraction of mass in bound structures increases with the effective density of the tracer, the surface density and mass of the structures, and the distance from the center of a galaxy. For the most complete surveys of structures in the Galaxy defined by CO J = 1 → 0, the fraction of mass that is in bound structures is 0.19. For catalogs of other galaxies based on CO J = 2 → 1, the fraction is 0.35. These results offer substantial alleviation of the fundamental problem of slow star formation. If only clouds found to be bound are counted and they are assumed to collapse in a freefall time at their mean cloud density, the sum over all clouds in a complete survey of the Galaxy yields a predicted star formation rate of 46 M⊙ yr−1, a factor of 6.5 less than if all clouds are bound.es_ES
Idiomadc.language.isoenes_ES
Publicadordc.publisherIOPes_ES
Tipo de licenciadc.rightsAttribution-NonCommercial-NoDerivs 3.0 United States*
Link a Licenciadc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/us/*
Fuentedc.sourceThe Astrophysical Journales_ES
Palabras clavesdc.subjectStar-formation ratees_ES
Palabras clavesdc.subjectOb associationses_ES
Palabras clavesdc.subjectMilky-wayes_ES
Palabras clavesdc.subjectGalactic distributiones_ES
Palabras clavesdc.subjectPhysical-propertieses_ES
Palabras clavesdc.subjectDense clumpses_ES
Palabras clavesdc.subjectCo surveyes_ES
Palabras clavesdc.subjectGases_ES
Palabras clavesdc.subjectTurbulencees_ES
Palabras clavesdc.subjectRegionses_ES
Títulodc.titleWhich molecular cloud structures are bound?es_ES
Tipo de documentodc.typeArtículo de revistaes_ES
dc.description.versiondc.description.versionVersión publicada - versión final del editores_ES
dcterms.accessRightsdcterms.accessRightsAcceso abiertoes_ES
Catalogadoruchile.catalogadorcrbes_ES
Indizaciónuchile.indexArtículo de publícación WoSes_ES


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Attribution-NonCommercial-NoDerivs 3.0 United States
Excepto si se señala otra cosa, la licencia del ítem se describe como Attribution-NonCommercial-NoDerivs 3.0 United States