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dc.contributor.authorRivilla, V. M.
dc.contributor.authorChandler, C. J.
dc.contributor.authorSanz-Forcada, J.
dc.contributor.authorJiménez-Serra, I.
dc.contributor.authorForbrich, J.
dc.contributor.authorMartín-Pintado, J.
dc.date.accessioned2017-07-13T17:06:44Z
dc.date.available2017-07-13T17:06:44Z
dc.date.issued2015-04-03
dc.identifier.citationRivilla , V M , Chandler , C J , Sanz-Forcada , J , Jiménez-Serra , I , Forbrich , J & Martín-Pintado , J 2015 , ' Short- and long-term variability of young stars in the Orion Nebula Cluster and Molecular Cloud ' , The Astrophysical Journal , vol. 808 , no. 2 . https://doi.org/10.1088/0004-637X/808/2/146
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 11212036
dc.identifier.otherPURE UUID: 933365fb-b4e9-4441-95f3-303eb5b1e1b3
dc.identifier.otherArXiv: http://arxiv.org/abs/1504.00849v1
dc.identifier.otherScopus: 84942116478
dc.identifier.urihttp://hdl.handle.net/2299/18931
dc.descriptionV. M. Rivilla, et al., “Short- and Long-term Radio Variability of Young Stars in the Orion Nebula Cluster and Molecular Cloud”, The Astrophysical Journal, Vol. 808(2), July 2015. © 2015. The American Astronomical Society. All rights reserved.
dc.description.abstractWe used the Very Large Array to carry out a multi-epoch radio continuum monitoring of the Orion Nebula Cluster and Orion Molecular Cloud. Our observations reveal the presence of 19 sources. With the exception of the sources BN and C the sources show variability between the different epochs. We have found tentative evidence of variability in the massive object related with source I. Our observations also confirm radio flux density variations of a factor >2 on timescales of hours to days in 5 sources. One of these flaring sources, OHC-E, has been detected for the first time. We conclude that the radio emission arises from: i) highly-variable non-thermal gyrosynchrotron emission produced by electrons accelerated in the magnetospheres of pre-main sequence stars; ii) thermal emission from ionized gas and/or heated dust around massive objects and proplyds. Combining our sample with other radio monitoring and a X-ray catalog, we have studied the properties of 51 radio/X-ray stars. We have found severals hints of a direct relation between the X-ray activity and the mechanisms responsible for (at least some fraction of) the radio emission. We have estimated a radio flaring rate of 0.14 flares day-1 in the densest stellar cluster of the region, suggesting that radio flares from young stars are more common events than previously thought.en
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectastro-ph.SR
dc.titleShort- and long-term variability of young stars in the Orion Nebula Cluster and Molecular Clouden
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/808/2/146
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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