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dc.contributor.authorCostigan, G.
dc.contributor.authorVink, Jorick S.
dc.contributor.authorScholz, A.
dc.contributor.authorRay, T.
dc.contributor.authorTesti, L.
dc.identifier.citationCostigan , G , Vink , J S , Scholz , A , Ray , T & Testi , L 2014 , ' Temperaments of young stars : rapid mass accretion rate changes in T Tauri and Herbig Ae stars ' Monthly Notices of the Royal Astronomical Society , vol. 440 , no. 4 , pp. 3444-3461 . DOI: 10.1093/mnras/stu529en
dc.identifier.otherPURE: 145105205
dc.identifier.otherPURE UUID: 625dc0f6-d689-45ff-9707-6f31c48a3ec2
dc.identifier.otherBibCode: 2014MNRAS.440.3444C
dc.identifier.otherScopus: 84899817805
dc.descriptionJSV would like to thank the UK Science and Technologies Facility Council (STFC) and the Northern Ireland Department of Culture Arts and Leisure (DCAL) for financial support. AS and TR would like to thank the Science Foundation of Ireland (SFI) for their support under grant numbers 11/RFP/AST/3331 and 10/RFP/AST2780.en
dc.description.abstractVariability in emission lines is a characteristic feature in young stars and can be used as a tool to study the physics of the accretion process. Here, we present a study of Hα variability in 15 T Tauri and Herbig Ae stars (K7 - B2) over a wide range of time windows, from minutes, to hours, to days, and years. We assess the variability using linewidth measurements and the time series of line profiles. All objects show gradual, slow profile changes on time-scales of days. In addition, in three cases there is evidence for rapid variations in Hα with typical time-scales of 10 min, which occurs in 10 per cent of the total covered observing time. The mean accretion rate changes, inferred from the line fluxes, are 0.01–0.07 dex for time-scales of <1 h, 0.04–0.4 dex for time-scales of days, and 0.13–0.52 dex for time-scales of years. In Costigan et al., we derived an upper limit finding that the intermediate (days) variability dominated over longer (years) variability. Here, our new results, based on much higher cadence observations, also provide a lower limit to accretion rate variability on similar time-scales (days), thereby constraining the accretion rate variability physics in a much more definitive way. A plausible explanation for the gradual variations over days is an asymmetric accretion flow resulting in a rotational modulation of the accretion-related emission, although other interpretations are possible as well. In conjunction with our previous work, we find that the time-scales and the extent of the variability is similar for objects ranging in mass from ∼0.1 to ∼5 M⊙. This confirms that a single mode of accretion is at work from T Tauri to Herbig Ae stars – across a wide range of stellar masses.en
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectAccretion discsen
dc.subjectStars: pre-main-sequenceen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleTemperaments of young stars : rapid mass accretion rate changes in T Tauri and Herbig Ae starsen
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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