Gaia21bty: An EXor light curve exhibiting a FUor spectrum

J 2023

Gaia21bty: An EXor light curve exhibiting a FUor spectrum

SIWAK, Michal, Lynne A HILLENBRAND, Agnes KOSPAL, Peter ABRAHAM, Teresa GIANNINI et. al.

Základní údaje

Originální název

Gaia21bty: An EXor light curve exhibiting a FUor spectrum

Autoři

SIWAK, Michal (616 Polsko), Lynne A HILLENBRAND, Agnes KOSPAL, Peter ABRAHAM, Teresa GIANNINI, Kishalay DE, Attila MOOR, Mate SZILAGYI, Jan JANÍK (203 Česká republika, garant, domácí), Chris KOEN, Sunkyung PARK, Zsofia NAGY, de Miera Fernando CRUZ-SAENZ, Eleonora FIORELLINO, Gabor MARTON, Maria KUN, Philip W LUCAS, Andrzej UDALSKI a Zsofia Marianna SZABO

Vydání

Monthly Notices of the Royal Astronomical Society, Oxford University Press, 2023, 0035-8711

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Velká Británie a Severní Irsko

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL URL

Impakt faktor

Impact factor: 4.800 v roce 2022

Kód RIV

RIV/00216224:14310/23:00131685

Organizační jednotka

Přírodovědecká fakulta

DOI

http://dx.doi.org/10.1093/mnras/stad2135

UT WoS

001048593700007

Klíčová slova anglicky

accretion; accretion discs; stars: formation; stars: pre-main-sequence; stars: variables: T Tauri; Herbig Ae/Be

Štítky

rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 26. 9. 2023 15:59, Mgr. Marie Šípková, DiS.

Anotace

V originále

Gaia21bty, a pre-main-sequence star that previously had shown aperiodic dips in its light curve, underwent a considerable Delta G approximate to 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 similar to 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-circle dot and the mass accretion rate is 2.5 x 10(-5) M-circle dot yr(-1), which are typical values for FUors even considering the large uncertainty in the distance (1.7(-0.4)(+0.8) 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.

Citovat

SIWAK, Michal, Lynne A HILLENBRAND, Agnes KOSPAL, Peter ABRAHAM, Teresa GIANNINI, Kishalay DE, Attila MOOR, Mate SZILAGYI, Jan JANÍK, Chris KOEN, Sunkyung PARK, Zsofia NAGY, de Miera Fernando CRUZ-SAENZ, Eleonora FIORELLINO, Gabor MARTON, Maria KUN, Philip W LUCAS, Andrzej UDALSKI a Zsofia Marianna SZABO. Gaia21bty: An EXor light curve exhibiting a FUor spectrum. Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2023, roč. 524, č. 4, s. 5548-5565. ISSN 0035-8711. Dostupné z: https://dx.doi.org/10.1093/mnras/stad2135.

@article{2310402,
   author = {Siwak, Michal and Hillenbrand, Lynne A and Kospal, Agnes and Abraham, Peter and Giannini, Teresa and De, Kishalay and Moor, Attila and Szilagyi, Mate and Janík, Jan and Koen, Chris and Park, Sunkyung and Nagy, Zsofia and CruzandSaenz, de Miera Fernando and Fiorellino, Eleonora and Marton, Gabor and Kun, Maria and Lucas, Philip W and Udalski, Andrzej and Szabo, Zsofia Marianna},
   article_number = {4},
   doi = {http://dx.doi.org/10.1093/mnras/stad2135},
   keywords = {accretion; accretion discs; stars: formation; stars: pre-main-sequence; stars: variables: T Tauri; Herbig Ae/Be},
   language = {eng},
   issn = {0035-8711},
   journal = {Monthly Notices of the Royal Astronomical Society},
   title = {Gaia21bty: An EXor light curve exhibiting a FUor spectrum},
   url = {https://academic.oup.com/mnras/article/524/4/5548/7226206},
   volume = {524},
   year = {2023}
}

TY  - JOUR
ID  - 2310402
AU  - Siwak, Michal - Hillenbrand, Lynne A - Kospal, Agnes - Abraham, Peter - Giannini, Teresa - De, Kishalay - Moor, Attila - Szilagyi, Mate - Janík, Jan - Koen, Chris - Park, Sunkyung - Nagy, Zsofia - Cruz-Saenz, de Miera Fernando - Fiorellino, Eleonora - Marton, Gabor - Kun, Maria - Lucas, Philip W - Udalski, Andrzej - Szabo, Zsofia Marianna
PY  - 2023
TI  - Gaia21bty: An EXor light curve exhibiting a FUor spectrum
JF  - Monthly Notices of the Royal Astronomical Society
VL  - 524
IS  - 4
SP  - 5548-5565
EP  - 5548-5565
PB  - Oxford University Press
SN  - 00358711
KW  - accretion
KW  - accretion discs
KW  - stars: formation
KW  - stars: pre-main-sequence
KW  - stars: variables: T Tauri
KW  - Herbig Ae/Be
UR  - https://academic.oup.com/mnras/article/524/4/5548/7226206
N2  - Gaia21bty, a pre-main-sequence star that previously had shown aperiodic dips in its light curve, underwent a considerable Delta G approximate to 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 similar to 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-circle dot and the mass accretion rate is 2.5 x 10(-5) M-circle dot yr(-1), which are typical values for FUors even considering the large uncertainty in the distance (1.7(-0.4)(+0.8) 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.
ER  -

SIWAK, Michal, Lynne A HILLENBRAND, Agnes KOSPAL, Peter ABRAHAM, Teresa GIANNINI, Kishalay DE, Attila MOOR, Mate SZILAGYI, Jan JANÍK, Chris KOEN, Sunkyung PARK, Zsofia NAGY, de Miera Fernando CRUZ-SAENZ, Eleonora FIORELLINO, Gabor MARTON, Maria KUN, Philip W LUCAS, Andrzej UDALSKI a Zsofia Marianna SZABO. Gaia21bty: An EXor light curve exhibiting a FUor spectrum. \textit{Monthly Notices of the Royal Astronomical Society}. Oxford University Press, 2023, roč.~524, č.~4, s.~5548-5565. ISSN~0035-8711. Dostupné z: https://dx.doi.org/10.1093/mnras/stad2135.

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