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Evolution of the optical emission lines and the X-ray emission during the super-active stage of T CrB
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abstract
T CrB is a symbiotic star that experiences nova outbursts every $\sim$ 80~yr. The next, long-anticipated nova outburst should occur during the 2024-2026 period. Here, we present results of high-resolution optical spectroscopy of T CrB in the period 2016 - 2023. In these spectra, we measured the equivalent widths of the H$\alpha$, H$\beta$, HeI and HeII emission lines. The maximum equivalent width (EW) was recorded on May 2021, when the EW of $H\alpha$ reached -44.6 \AA and H$\beta$ = -21.5 \AA. At the other extreme, the minimum of EW($H\alpha$)= -2.9 \AA was recorded in October 2023. After October 2023, the B-band emission brightened, suggesting a re-appearance of the orbital modulation. In addition to the optical data, we study the X-ray behaviour in the same period. We find a strong correlation between $EW(H\alpha)$ and X-ray flux with a correlation coefficient -0.78 and a significance of 2.6$\times 10^{-5}$.
Forward citations
Cited by 2 Pith papers
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Modeling the high-brightness state of the recurrent nova T CrB as an enhanced mass-transfer event
T CrB's 15-year brightening is best explained by a temporary hundredfold increase in mass transfer onto a high-viscosity disk, with the pre-eruption dip caused by an inner disk edge expanding at 0.02 km/s.
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When will T Coronae Borealis next erupt as a nova? Constraints from recurrence, orbital phase, and accretion-state evolution
T CrB's next eruption is not uniquely predictable; conditional scenarios point to a possible 2026 December eruption if the current decline mimics 1946, or a lower limit near 2029 May if the recent high state left an a...
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