المستودع الأكاديمي جامعة المدينة

Anatomy of HH 111 from CO Observations: a Bow-shock-driven Molecular Outflow

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dc.creator Lefloch, Bertrand
dc.creator Cernicharo, José
dc.creator Reipurth, Jo
dc.creator Pardo Carrión, Juan Ramón
dc.creator Neri, Roberto
dc.date 2007-12-28T12:52:24Z
dc.date 2007-12-28T12:52:24Z
dc.date 2007-03-20
dc.date.accessioned 2017-01-31T00:59:35Z
dc.date.available 2017-01-31T00:59:35Z
dc.identifier The Astrophysical Journal, 658: 498-508 (2007)
dc.identifier 1538-4357
dc.identifier http://hdl.handle.net/10261/2638
dc.identifier 10.1086/509600
dc.identifier.uri http://dspace.mediu.edu.my:8181/xmlui/handle/10261/2638
dc.description We present single-dish and interferometric millimeter line observations of the HH 111 outflow and its driving source. The physical conditions of the core have been determined from the emission of the millimeter line of CO and its isotopomers and CS with the IRAM 30 m telescope, and the CO J=7-->6 line with the Caltech Submillimeter Observatory. The emission reveals a small condensation of cold (T=20-25 K) and dense gas [n(H2)=3x10^5 cm^-3]. The outflow has been mapped with the IRAM Plateau de Bure Interferometer (PdBI). The cold gas is distributed in a hollow cylinder surrounding the optical jet. The formation of this cavity and its kinematics are well accounted for in the frame of outflow gas entrainment by jet bow shocks. Evidence of gas acceleration is found along the cavity walls, correlated with the presence of optical bow shocks. The separation of the inner walls reaches 8"-10", which matches the transverse size of the wings in the bow shock. CSO observations of the J=7-->6 line show evidence of a high-velocity and hot gas component (T=300-1000 K) with a low filling factor. This emission probably arises from shocked gas in the jet. Observations of the 3P2-3P1 [CI] line are consistent with C-type nondissociative shocks. Mapping of the high-velocity molecular bullets B1-B3, located beyond the optical jet, reveals small structures of 3" x 7" flattened perpendicular to the flow direction. They are made of cold (T ~ 30K), moderate density gas [n(H2) = (0.5-1.0)x10^4 cm^-3], expanding into the low-density surrounding medium. Their properties are consistent with their being shocked gas knots resulting from past time-variable ejections in the jet.
dc.description Peer reviewed
dc.format 1373320 bytes
dc.format application/pdf
dc.language eng
dc.publisher American Astronomical Society
dc.publisher University of Chicago Press
dc.rights openAccess
dc.subject ISM: clouds
dc.subject ISM: individual (HH 111)
dc.subject ISM: jets and outflows
dc.subject Stars: formation
dc.title Anatomy of HH 111 from CO Observations: a Bow-shock-driven Molecular Outflow
dc.type Artículo


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