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Authordc.contributor.authorPurser, S. J. D. 
Authordc.contributor.authorLumsden, S. L. 
Authordc.contributor.authorHoare, M. G. 
Authordc.contributor.authorUrquhart, J. S. 
Authordc.contributor.authorCunningham, N. 
Authordc.contributor.authorPurcell, C. R. 
Authordc.contributor.authorBrooks, K. J. 
Authordc.contributor.authorGaray Brignardello, Guido 
Authordc.contributor.authorGuzmán Fernández, Andrés 
Authordc.contributor.authorVoronkov, M. A. 
Admission datedc.date.accessioned2016-12-27T14:57:09Z
Available datedc.date.available2016-12-27T14:57:09Z
Publication datedc.date.issued2016
Cita de ítemdc.identifier.citationMNRAS 460, 1039–1053 (2016)es_ES
Identifierdc.identifier.other10.1093/mnras/stw1027
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/142117
Abstractdc.description.abstractRadio continuum observations using the Australia telescope compact array at 5.5, 9.0, 17.0 and 22.8 GHz have detected free-free emission associated with 45 of 49 massive young stellar objects and H ii regions. Of these, 26 sources are classified as ionized jets (12 of which are candidates), 2 as ambiguous jets or disc winds, 1 as a disc-wind, 14 as H ii regions and 2 were unable to be categorized. Classification as ionized jets is based upon morphology, radio flux and spectral index, in conjunction with previous observational results at other wavelengths. Radio luminosity and momentum are found to scale with bolometric luminosity in the same way as low-mass jets, indicating a common mechanism for jet production across all masses. In 13 of the jets, we see associated non-thermal/optically thin lobes resulting from shocks either internal to the jet and/or at working surfaces. 10 jets display non-thermal (synchrotron emission) spectra in their lobes, with an average spectral index of alpha = -0.55 consistent with Fermi acceleration in shocks. This shows that magnetic fields are present, in agreement with models of jet formation incorporating magnetic fields. Since the production of collimated radio jets is associated with accretion processes, the results presented in this paper support the picture of disc-mediated accretion for the formation of massive stars with an upper limit on the jet phase lasting approximately 6.5 x 10(4) yr. Typical mass-loss rates in the jet are found to be 1.4 x 10(-5) M-aS (TM) yr(-1) with associated momentum rates of the order of (1-2) x 10(-2) M-aS (TM) km s(-1) yr(-1)es_ES
Patrocinadordc.description.sponsorshipScience and Technology Facilities Council of the United Kingdom (STFC) FONCEDYT 3150570 Science and Technology Facilities Council of the United Kingdomes_ES
Lenguagedc.language.isoenes_ES
Publisherdc.publisherOxford University Presses_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/cl/*
Sourcedc.sourceMonthly Notices of the Royal Astronomical Societyes_ES
Keywordsdc.subjectStars: evolutiones_ES
Keywordsdc.subjectStars: formationes_ES
Keywordsdc.subjectStars: massivees_ES
Keywordsdc.subjectStars: protostarses_ES
Keywordsdc.subjectISM: jets and outflowses_ES
Keywordsdc.subjectRadio continuum: ISMes_ES
Títulodc.titleA search for ionized jets towards massive young stellar objectses_ES
Document typedc.typeArtículo de revista
Catalogueruchile.catalogadorapces_ES
Indexationuchile.indexArtículo de publicación ISIes_ES


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Attribution-NonCommercial-NoDerivs 3.0 Chile
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile