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dc.contributor.authorBozhinova, Inna Nikolaeva
dc.contributor.authorScholz, Alexander
dc.contributor.authorEislöffel, J.
dc.identifier.citationBozhinova , I N , Scholz , A & Eislöffel , J 2016 , ' Variability in young very low mass stars : two surprises from spectrophotometric monitoring ' , Monthly Notices of the Royal Astronomical Society , vol. 458 , no. 3 , pp. 3118-3133 .
dc.identifier.otherPURE: 241842658
dc.identifier.otherPURE UUID: 623dc622-e0a7-4a43-8c00-c65af44891ce
dc.identifier.otherBibCode: 2016MNRAS.tmp..284B
dc.identifier.otherScopus: 84964735365
dc.identifier.otherWOS: 000375799000061
dc.descriptionThe authors acknowledge support from the Science & Technology Facilities Council through grants no. ST/K502339/1 and ST/M001296/1.en
dc.description.abstractWe present simultaneous photometric and spectroscopic observations of seven young and highly variable M dwarfs in star-forming regions in Orion, conducted in four observing nights with FOcal Reducer and low dispersion Spectrograph2 at European Southern Observatory/VLT. All seven targets show significant photometric variability in the I band, with amplitudes between 0.1–0.8 mag, The spectra, however, remain remarkably constant, with spectral type changes less than 0.5 subtypes. Thus, the brightness changes are not caused by veiling that ‘fills in’ absorption features. Three objects in the σ Ori cluster (age ∼3 Myr) exhibit strong Hα emission and Hα variability, in addition to the continuum variations. Their behaviour is mostly consistent with the presence of spots with temperature of ∼300 K above the photosphere and filling factors between 0.2–0.4, in contrast to typical hotspots observed in more massive stars. The remaining targets near ϵ Ori, likely to be older, show eclipse-like light curves, no significant Hα activity and are better represented by variable extinction due to circumstellar material. Interestingly, two of them show no evidence of infrared excess emission. Our study shows that high-amplitude variability in young very low mass stars can be caused by different phenomena than in more massive T Tauri stars and can persist when the disc has disappeared and accretion has ceased.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at:
dc.subjectBrown dwarfsen
dc.subjectStars: low-massen
dc.subjectStars: pre-main-sequenceen
dc.subjectStars: variables: T Taurien
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleVariability in young very low mass stars : two surprises from spectrophotometric monitoringen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.description.statusPeer revieweden

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