20 research outputs found
Gaia21bty: An EXor lightcurve exhibiting an FUor spectrum
Gaia21bty, a pre-main sequence star that previously had shown aperiodic dips
in its light curve, underwent a considerable mag
brightening that occurred over a few months between 2020 October - 2021
February. The Gaia lightcurve shows that the star remained near maximum
brightness for about months, and then started slowly fading over the next
2 years, with at least three superimposed 1 mag sudden rebrightening
events. Whereas the amplitude and duration of the maximum is typical for EXors,
optical and near-infrared spectra obtained at the maximum are dominated by
features which are typical for FUors. Modelling of the accretion disc at the
maximum indicates that the disc bolometric luminosity is 43 L and the
mass accretion rate is M yr, which are
typical values for FUors even considering the large uncertainty in the distance
( 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 multi-colour 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.Comment: Accepted to MNRA
Photometric and spectroscopic study of the burst-like brightening of two Gaia-alerted young stellar objects
Young stars show variability on different time-scales from hours to decades,
with a range of amplitudes. We studied two young stars, which triggered the
Gaia Science Alerts system due to brightenings on a time-scale of a year.
Gaia20bwa brightened by about half a magnitude, whereas Gaia20fgx brightened by
about two and half magnitudes. We analyzed the Gaia light curves, additional
photometry, and spectra taken with the Telescopio Nazionale Galileo and the
Gran Telescopio Canarias. Several emission lines were detected toward
Gaia20bwa, including hydrogen lines from H to H, Pa,
Br, and lines of Ca II, O I, and Na I. The H and Br
lines were detected toward Gaia20fgx in emission in its bright state, with
additional CO lines in absorption, and the Pa line with an inverse P
Cygni profile during its fading. Based on the Br lines the accretion
rate was yr for Gaia20bwa and
yr for Gaia20fgx during their bright
state. The accretion rate of Gaia20fgx dropped by almost a factor of 10 on a
time-scale of half a year. The accretion parameters of both stars were found to
be similar to those of classical T Tauri stars, lower than those of young
eruptive stars. However, the amplitude and time-scale of these brightenings
place these stars to a region of the parameter space, which is rarely populated
by young stars. This suggests a new class of young stars, which produce
outbursts on a time-scale similar to young eruptive stars, but with smaller
amplitudes.Comment: Accepted to MNRA
Gaia21bty: An EXor lightcurve exhibiting an FUor spectrum
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 - 2021 February. The Gaia lightcurve shows that the star remained near maximum brightness for about 4 - 6 months, and then started slowly fading over the next 2 years, with at least three superimposed ~1 mag sudden rebrightening events. Whereas the amplitude and duration of the maximum is typical for EXors, optical and near-infrared spectra obtained at the maximum are dominated by features which are typical for 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 ( 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 multi-colour 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
Photometric and spectroscopic study of the EXor-like eruptive young star Gaia19fct
Funding: This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program under grant agreement No. 716155 (SACCRED) and from the "Transient Astrophysical Objects" GINOP 2.3.2-15-2016-00033 project of the National Research, Development and Innovation Office (NKFIH), Hungary, funded by the European Union. We acknowledge support from ESA PRODEX contract No. 4000132054. Zs.N., L.K., and K.V. acknowledge the support by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences. K.V. is supported by the Bolyai+ grant UNKP-22-5-ELTE-1093. This project has been supported by the K-131508 grant of the Hungarian National Research, Development and Innovation Office (NKFIH) and the Élvonal grant KKP-143986. Authors acknowledge the financial support of the Austrian-Hungarian Action Foundation (101.u13, 104.u2). L.K. acknowledges the financial support of the Hungarian National Research, Development and Innovation Office grant NKFIH PD-134784. This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004719 (OPTICON-RadioNet Pilot).Gaia19fct is one of the Gaia-alerted eruptive young stars that has undergone several brightening events. We conducted monitoring observations using multifilter optical and near-infrared photometry, as well as near-infrared spectroscopy, to understand the physical properties of Gaia19fct and investigate whether it fits into the historically defined two classes. We present the analyses of light curves, color variations, spectral lines, and CO modeling. The light curves show at least five brightening events since 2015, and the multifilter color evolutions are mostly gray. The gray evolution indicates that bursts are triggered by mechanisms other than extinction. Our near-infrared spectra exhibit both absorption and emission lines and show time variability throughout our observations. We found lower rotational velocity and lower temperature from the near-infrared atomic absorption lines than from the optical lines, suggesting that Gaia19fct has a Keplerian rotating disk. The CO overtone features show a superposition of absorption and emission components, which is unlike other young stellar objects. We modeled the CO lines, and the result suggests that the emission and absorption components are formed in different regions. We found that although Gaia19fct exhibits characteristics of both types of eruptive young stars, FU Orionis–type objects and EX Lupi–type objects, it shows more similarity with EXors in general.Publisher PDFPeer reviewe
Photometric and spectroscopic study of the EXor-like eruptive young star Gaia19fct
This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program under grant agreement No. 716155 (SACCRED) and from the "Transient Astrophysical Objects" GINOP 2.3.2-15-2016-00033 project of the National Research, Development and Innovation Office (NKFIH), Hungary, funded by the European Union. We acknowledge support from ESA PRODEX contract No. 4000132054. Zs.N., L.K., and K.V. acknowledge the support by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences. K.V. is supported by the Bolyai+ grant UNKP-22-5-ELTE-1093. This project has been supported by the K-131508 grant of the Hungarian National Research, Development and Innovation Office (NKFIH) and the Élvonal grant KKP-143986. Authors acknowledge the financial support of the Austrian-Hungarian Action Foundation (101.u13, 104.u2). L.K. acknowledges the financial support of the Hungarian National Research, Development and Innovation Office grant NKFIH PD-134784. This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004719 (OPTICON-RadioNet Pilot).Gaia19fct is one of the Gaia-alerted eruptive young stars that has undergone several brightening events. We conducted monitoring observations using multifilter optical and near-infrared photometry, as well as near-infrared spectroscopy, to understand the physical properties of Gaia19fct and investigate whether it fits into the historically defined two classes. We present the analyses of light curves, color variations, spectral lines, and CO modeling. The light curves show at least five brightening events since 2015, and the multifilter color evolutions are mostly gray. The gray evolution indicates that bursts are triggered by mechanisms other than extinction. Our near-infrared spectra exhibit both absorption and emission lines and show time variability throughout our observations. We found lower rotational velocity and lower temperature from the near-infrared atomic absorption lines than from the optical lines, suggesting that Gaia19fct has a Keplerian rotating disk. The CO overtone features show a superposition of absorption and emission components, which is unlike other young stellar objects. We modeled the CO lines, and the result suggests that the emission and absorption components are formed in different regions. We found that although Gaia19fct exhibits characteristics of both types of eruptive young stars, FU Orionis–type objects and EX Lupi–type objects, it shows more similarity with EXors in general.Publisher PDFPeer reviewe
The Gaia alerted fading of the FUor-type star Gaia21elv
FU Orionis objects (FUors) are eruptive young stars, which exhibit outbursts
that last from decades to a century. Due to the duration of their outbursts,
and to the fact that only about two dozens of such sources are known,
information on the end of their outbursts is limited. Here we analyse follow-up
photometry and spectroscopy of Gaia21elv, a young stellar object, which had a
several decades long outburst. It was reported as a Gaia science alert due to
its recent fading by more than a magnitude. To study the fading of the source
and look for signatures characteristic of FUors, we have obtained follow-up
near infrared (NIR) spectra using Gemini South/IGRINS, and both optical and NIR
spectra using VLT/X-SHOOTER. The spectra at both epochs show typical FUor
signatures, such as a triangular shaped -band continuum, absorption-line
dominated spectrum, and P Cygni profiles. In addition to the typical FUor
signatures, [OI], [FeII], and [SII] were detected, suggesting the presence of a
jet or disk wind. Fitting the spectral energy distributions with an accretion
disc model suggests a decrease of the accretion rate between the brightest and
faintest states. The rapid fading of the source in 2021 was most likely
dominated by an increase of circumstellar extinction. The spectroscopy
presented here confirms that Gaia21elv is a classical FUor, the third such
object discovered among the Gaia science alerts.Comment: Accepted to MNRA