A population of eruptive variable protostars in VVV

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dc.contributor.authorContreras Peña, C.
dc.contributor.authorLucas, P.W.
dc.contributor.authorMinniti, D.
dc.contributor.authorKurtev, R.
dc.contributor.authorStimson, W.
dc.contributor.authorNavarro Molina, C.
dc.contributor.authorBorissova, J.
dc.contributor.authorKumar, M.S.N.
dc.contributor.authorThompson, M.A.
dc.contributor.authorGledhill, T.
dc.contributor.authorTerzi, R.
dc.contributor.authorFroebrich, D.
dc.contributor.authorCaratti o Garatti, A.
dc.date.accessioned2017-09-14T20:16:27Z
dc.date.available2017-09-14T20:16:27Z
dc.date.issued2016-11
dc.descriptionIndexación: Web of Science; Scopus.es_CL
dc.description.abstractWe present the discovery of 816 high-amplitude infrared variable stars (ΔKs > 1 mag) in 119 deg2 of the Galactic mid-plane covered by the VISTA Variables in the Via Lactea (VVV) survey. Almost all are new discoveries and about 50 per cent are young stellar objects (YSOs). This provides further evidence that YSOs are the commonest high-amplitude infrared variable stars in the Galactic plane. In the 2010-2014 time series of likely YSOs, we find that the amplitude of variability increases towards younger evolutionary classes (class I and flatspectrum sources) except on short time-scales (< 25 d) where this trend is reversed. Dividing the likely YSOs by light-curve morphology, we find 106 with eruptive light curves, 45 dippers, 39 faders, 24 eclipsing binaries, 65 long-term periodic variables (P > 100 d) and 162 shortterm variables. Eruptive YSOs and faders tend to have the highest amplitudes and eruptive systems have the reddest spectral energy distribution (SEDs). Follow-up spectroscopy in a companion paper verifies high accretion rates in the eruptive systems. Variable extinction is disfavoured by the two epochs of colour data. These discoveries increase the number of eruptive variable YSOs by a factor of at least 5, most being at earlier stages of evolution than the known FUor and EXor types. We find that eruptive variability is at least an order of magnitude more common in class I YSOs than class II YSOs. Typical outburst durations are 1-4 yr, between those of EXors and FUors. They occur in 3-6 per cent of class I YSOs over a 4 yr time spanes_CL
dc.description.urihttps://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw2801
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Volume 465, Issue 3, 1 March 2017, Pages 3011–3038es_CL
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.otherhttps://doi.org/10.1093/mnras/stw2801
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/4246
dc.language.isoenes_CL
dc.publisherOXFORD UNIV PRESSes_CL
dc.subjectHerbig Ae/Bees_CL
dc.subjectInfrared: starses_CL
dc.subjectStars: AGB and post-AGBes_CL
dc.subjectStars: low-masses_CL
dc.subjectStars: pre-main-sequencees_CL
dc.subjectStars: protostarses_CL
dc.subjectStars: variables: T Tauries_CL
dc.titleA population of eruptive variable protostars in VVVes_CL
dc.typeArtículoes_CL
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