An UXor among FUors: Extinction-related Brightness Variations of the Young Eruptive Star V582 Aur

Ábrahám, P.; Kóspál, Á.; Kun, M.; Fehér, Orsolya; Zsidi, Gabriella; Acosta–Pulido, J. A.; Carnerero, M. I.; García-Álvarez, D.; Moór, A.; Cseh, B.; Hajdu, G.; Hanyecz, O.; Kelemen, J.; Kriskovics, L.; Márton, G.; Mez, Gy; Molnár, L.; Ordasi, A.; Rodríguez-Coira, G.; Sárneczky, K.; Sódor,; Szakáts, R.; Szegedi-Elek, E.; Szing, A.; Farkas-Takács, Anikó; Vida, K.; Vinkó, J.

doi:10.3847/1538-4357/aaa242

Cited by 24 publications

(7 citation statements)

References 39 publications

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“…For example, V960 Mon, in which the brightness decreases by 2 stellar magnitudes in the V-band for a period of about five years [44]. In the case of V582 Aur two deep decreases in brightens by about 3 magnitudes in R-band have been observed separated by a five-year period [45,46]. In the case of V582 Aur, two deep declines in brightens of about 3 stellar magnitudes in the Rband were observed, five years apart.…”

Section: Discussionmentioning

confidence: 98%

The FUor Star V2493 Cyg (HBC 722)—Eleven Years at Maximum Brightness

2021

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At the time of stellar evolution, young stellar objects go through processes of increased activity and instability. Star formation takes place in several stages during which the star accumulates enough mass to initiate thermonuclear reactions in the nucleus. A significant percentage of the mass of Sun-like stars accumulates during periods of increased accretion known as FUor outbursts. Since we know only about two dozen stars of this type, the study of each new object is very important for our knowledge. In this paper, we present data from photometric monitoring on a FUor object V2493 Cyg discovered in 2010. Our data were obtained in the optical region with BVRI Johnson–Cousins set of filters during the period from November 2016 to February 2021. The results of our observations show that during this period no significant changes in the brightness of the star were registered. We only detect variations with a small amplitude around the maximum brightness value. Thus, since 2013 V2493 Cyg remains at its maximum brightness, without a decrease in brightness. Such photometric behavior is not typical of other stars from FUor type. Usually, the light curves of FUors are asymmetrical, with a very rapid rise and gradual decline of the brightness. V2493 Cyg remains unique in this respect with a very rapid rise in brightness and prolonged retention in maximum light. Our period analysis made for the interval February 2013–February 2021 reveals a well-defined period of 914 ± 10 days. Such periodicity can be explained by dust structures remaining from star formation in orbit around the star.

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Section: Discussionmentioning

confidence: 98%

The FUor Star V2493 Cyg (HBC 722)—Eleven Years at Maximum Brightness

2021

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“…The interferometric 13 CO and C 18 O survey of Fehér et al (2017) determines that V10 (V733 Cep) and V2 (HBC722) have evolved beyond the class I and flat-spectrum stages. Abrahám et al (2018) determines that the pre-outburst spectrum of V36 (V582 Aur) is that of a classical T Tauri star. There is no literature information in the case of V4, however the spectral index of α = −0.4 is an upper limit and makes this object a very likely class II YSO.…”

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confidence: 99%

Determining the recurrence time-scale of long-lasting YSO outbursts

Peña

Naylor

Morrell

2019

Monthly Notices of the Royal Astronomical Society

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We have determined the rate of large accretion events in class I and II young stellar objects (YSOs) by comparing the all-sky digitised photographic plate surveys provided by SuperCOSMOS with the latest data release from Gaia (DR2). The long mean baseline of 55 years along with a large sample of class II YSOs (≃15,000) allows us to study approximately 1 million YSO-years. We find 139 objects with ∆R ≥ 1 mag, most of which are found at amplitudes between 1 and 3 mag. The majority of YSOs in this group show irregular variability or long-lasting fading events, which is best explained as hot spots due to accretion or by variable extinction. There is a tail of YSOs at ∆R ≥ 3 mag and they seem to represent a different population. Surprisingly many objects in this group show high-amplitude irregular variability over timescales shorter than 10 years, in contrast with the view that high-amplitude objects always have long outbursts. However, we find 6 objects that are consistent with undergoing large, long lasting accretion events, 3 of them previously unknown. This yields an outburst recurrence timescale of 112 kyr, with a 68% confidence interval [74 to 180] kyr. This represents the first robust determination of the outburst rate in class II YSOs and shows that YSOs in their planet-forming stage do in fact undergo large accretion events, and with timescales of ≃100,000 years. In addition, we find that outbursts in the class II stage are ≃10 times less frequent than during the class I stage.

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“…Its brightening started between 1984 and 1985, it reached its maximum in 1986, and it is still close to maximum brightness (Semkov et al 2013). Its flat spectral energy distribution (SED) and millimeter observations indicate a significant amount of circumstellar material, including a massive envelope ( Ábrahám et al 2018;Zsidi et al 2019).…”

Section: Target Selectionmentioning

confidence: 99%

Grain growth in newly discovered young eruptive stars

Kóspál,

Ábrahám,

Carmona

et al. 2020

Preprint

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FU Orionis-type stars are young stellar objects showing large outbursts due to highly enhanced accretion from the circumstellar disk onto the protostar. FUor-type outbursts happen in a wide variety of sources from the very embedded ones to those with almost no sign of extended emission beyond the disk. The subsequent eruptions might gradually clear up the obscuring envelope material and drive the protostar on its way to become a disk-only T Tauri star. We used VLT/VISIR to obtain the first spectra that cover the 8 − 13 µm mid-infrared wavelength range in low-resolution of five recently discovered FUors. Four objects from our sample show the 10 µm silicate feature in emission. We study the shape and strength of the silicate feature in these objects and find that they mostly contain large amorphous grains, suggesting that large grains are typically not settled to the midplane in FUor disks. This is a general characteristic of FUors, as opposed to regular T Tauri-type stars whose disks display anything from pristine small grains to significant grain growth. We classify our targets by determining whether the silicate feature is in emission or in absorption, and confront them with the evolutionary scenarios on the dispersal of the envelopes around young stars. In our sample, all Class II objects exhibit silicate emission, while for Class I objects, the appearance of the feature in emission or absorption depends on the viewing angle with respect to the outflow cavity. This highlights the importance of geometric effects when interpreting the silicate feature.

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An UXor among FUors: Extinction-related Brightness Variations of the Young Eruptive Star V582 Aur

Cited by 24 publications

References 39 publications

The FUor Star V2493 Cyg (HBC 722)—Eleven Years at Maximum Brightness

The FUor Star V2493 Cyg (HBC 722)—Eleven Years at Maximum Brightness

Determining the recurrence time-scale of long-lasting YSO outbursts

Grain growth in newly discovered young eruptive stars

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