Gaia21bty : an EXor light curve exhibiting a FUor spectrum
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Gaia21bty, a pre-main-sequence star that previously had shown aperiodic dips in its light curve, underwent a considerable ΔG ≈ 2.9 mag brightening that occurred over a few months between 2020 October and 2021 February. The Gaia light curve shows that the star remained near maximum brightness for about 4–6 months, and then started slowly fading over the next 2 yr, with at least three superimposed ∼1 mag sudden rebrightening events. Whereas the amplitude and duration of the maximum is typical for EX Lupi-type stars, optical and near-infrared spectra obtained at the maximum are dominated by features which are typical for FU Ori-type stars (FUors). Modelling of the accretion disc at the maximum indicates that the disc bolometric luminosity is 43 L⊙ and the mass accretion rate is 2.5 × 10−5 M⊙ yr−1, which are typical values for FUors even considering the large uncertainty in the distance (1.7+0.8−0.4 kpc). Further monitoring is necessary to understand the cause of the quick brightness decline, the rebrightening, and the other post-outburst light changes, as our multicolour photometric data suggest that they could be caused by a long and discontinuous obscuration event. We speculate that the outburst might have induced large-scale inhomogeneous dust condensations in the line of sight leading to such phenomena, whilst the FUor outburst continues behind the opaque screen.
Siwak , M , Hillenbrand , L A , Kóspál , Á , Ábrahám , P , Giannini , T , De , K , Moór , A , Szilágyi , M , Janík , J , Koen , C , Park , S , Nagy , Z , Cruz-Sáenz de Miera , F , Fiorellino , E , Marton , G , Kun , M , Lucas , P W , Udalski , A & Szabo , Z M 2023 , ' Gaia21bty : an EXor light curve exhibiting a FUor spectrum ' , Monthly Notices of the Royal Astronomical Society , vol. 524 , no. 4 , pp. 5548–5565 . https://doi.org/10.1093/mnras/stad2135
Monthly Notices of the Royal Astronomical Society
Copyright © 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stad2135.
DescriptionFunding: This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 716155 (SACCRED). We acknowledge support from the ESA PRODEX Contract No. 4000132054. GM and ZN were supported by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences. GM acknowledges support from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004141. EF acknowledges financial support from the project PRIN-INAF 2019 ‘Spectroscopically Tracing the Disc Dispersal Evolution (STRADE)’. ZMS acknowledges funding from a St Leonards scholarship from the University of St Andrews.
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