Size of the accretion disc in the recurrent nova T CrB

2024/05/19 by R. K. Zamanov, Zamanov, R. K., K. A. Stoyanov +17 · 2 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #High-pressure geophysics and materials #Solar and Stellar Astrophysics (astro-ph.SR)

paper · pdf · doi:10.48550/arxiv.2405.11506

openalex publication_date 2024/05/19 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

We present high resolution (0.06 A/px) spectroscopic observations of the recurrent nova T Coronae Borealis obtained during the last 1.5 years (September 2022 -- January 2024), with the 2.0m RCC telecope of the Rozhen National Astronomical Observatory, Bulgaria. Double-peaked emission is visible in the H-alpha line after the end of the superactive state. We subtract the red giant contribution and measure the distance between the peaks (Δv_a) of the line. For the period July 2023 -- January 2024, we find that Δv_a is in range 90 < Δv_a < 120 km/s. Assuming that the emission is from the accretion disc around the white dwarf, we find average radius of the accretion disc R_disc = 89 ± 19 R_\odot, 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.

Cited by

• The pre-eruption state of T CrB as observed with ALMA in 2024
• Modeling the high-brightness state of the recurrent nova T CrB as an enhanced mass-transfer event

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