Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova

Iłkiewicz, Krystian; Mikołajewska, Joanna; Stoyanov, Kiril A.

doi:10.3847/2041-8213/ace9dc

Cited by 3 publications

(1 citation statement)

References 35 publications

(52 reference statements)

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“…However, their duration and amplitude depend mainly on the size of the accretion disk. In particular, their duration can range from a few days (e.g., Cannizzo et al 2012) to years (e.g., Iłkiewicz et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Classifying Optical (Out)bursts in Cataclysmic Variables: The Distinct Observational Characteristics of Dwarf Novae, Micronovae, Stellar Flares, and Magnetic Gating

Iłkiewicz,

Scaringi,

Veresvarska

et al. 2024

ApJL

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Cataclysmic variables can experience short optical brightenings, which are commonly attributed to phenomena such as dwarf novae outbursts, micronovae, donor flares, or magnetic gating bursts. Since these events exhibit similar observational characteristics, their identification has often been ambiguous. In particular, magnetic gating bursts and micronovae have been suggested as alternative interpretations of the same phenomena. Here we show that the timescales and energies separate the optical brightenings into separate clusters consistent with their different classifications. This suggests that micronovae and magnetic gating bursts are in fact separate phenomena. Based on our findings, we develop diagnostic diagrams that can distinguish between these bursts/flares based on their properties. We demonstrate the effectiveness of this approach on observations of a newly identified intermediate polar, CTCV J0333-4451, which we classify as a magnetic gating system. CTCV J0333-4451 is the third highest spin-to-orbital period ratio intermediate polar with magnetic gating, suggesting that these bursts are common among these rare systems.

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Section: Introductionmentioning

confidence: 99%

Classifying Optical (Out)bursts in Cataclysmic Variables: The Distinct Observational Characteristics of Dwarf Novae, Micronovae, Stellar Flares, and Magnetic Gating

Iłkiewicz,

Scaringi,

Veresvarska

et al. 2024

ApJL

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Size of the accretion disc in the recurrent nova T CrB

Zamanov,

Stoyanov,

Marchev

et al. 2024

Astron Nachr

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We present high‐resolution (0.06 Å px) spectroscopic observations of the recurrent nova T Coronae Borealis obtained during the last 1.5 years (September 2022–January 2024), with the 2.0‐m RCC telescope of the Rozhen National Astronomical Observatory, Bulgaria. Double‐peaked emission is visible in the line after the end of the superactive state. We subtract the red giant contribution and measure the distance between the peaks () of the line. For the period July 2023–January 2024, we find that is in range km s. Assuming that the emission is from the accretion disc around the white dwarf, we find average radius of the accretion disc R, which is approximately equal to the Roche lobe size of the white dwarf. Our results indicate that tidal torque plays an important role but that the disc can extend up to the Roche lobe of the accreting star.

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Accretion in the recurrent nova T CrB: Linking the superactive state to the predicted outburst

Zamanov,

Boeva,

Latev

et al. 2023

A&A

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Context. T CrB (NOVA CrB 1946) is a famous recurrent nova with a recurrence timescale of 80 years. Aims. We aim to estimate the colours, luminosity, and mass-accretion rate for T CrB (NOVA CrB 1946) during and after the superactive state. Methods. We performed and analysed UBV photometry of the recurrent nova T CrB. Results. For the hot component of T CrB, we find average dereddened colours of (U − B)0 = −0.70 ± 0.08 and (B − V)0 = 0.23 ± 0.06, which correspond to an effective temperature of 9400 ± 500 K and an optical luminosity of 40 − 110 L⊙ during the superactive state (2016–2022). After the end of the superactive state, the hot component became significantly redder, (U − B)0 ≈ −0.3 and (B − V)0 ≈ 0.6 in August 2023, and its luminosity decreased markedly to 20 − 25 L⊙ in April–May 2023, and to 8 − 9 L⊙ in August 2023. The total mass accreted during the superactive state from 2014 to 2023 is ∼2 × 10−7 M⊙. Conclusions. This is a significant fraction of the mass required to cause a thermonuclear runaway (TNR). Overall our results support a model in which a large accretion disc acts as a reservoir with increased accretion rate onto the central white dwarf during disc high states, ultimately leading to a TNR explosion, which now seems to be imminent.

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Symbiotic Star T CrB as an Extreme SU UMa–type Dwarf Nova

Cited by 3 publications

References 35 publications

Classifying Optical (Out)bursts in Cataclysmic Variables: The Distinct Observational Characteristics of Dwarf Novae, Micronovae, Stellar Flares, and Magnetic Gating

Classifying Optical (Out)bursts in Cataclysmic Variables: The Distinct Observational Characteristics of Dwarf Novae, Micronovae, Stellar Flares, and Magnetic Gating

Size of the accretion disc in the recurrent nova T CrB

Accretion in the recurrent nova T CrB: Linking the superactive state to the predicted outburst

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