Size of the accretion disc in the recurrent nova T CrB
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arXiv
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| Main Authors: | , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866909207060545536 |
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| author | Zamanov, R. K. Stoyanov, K. A. Marchev, V. Minev, M. Marchev, D. Moyseev, M. Marti, J. Bode, M. F. Konstantinova-Antova, R. Stefanov, S. |
| author_facet | Zamanov, R. K. Stoyanov, K. A. Marchev, V. Minev, M. Marchev, D. Moyseev, M. Marti, J. Bode, M. F. Konstantinova-Antova, R. Stefanov, S. |
| contents | 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 $R_{disc} = 89 \pm 19$ 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. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2405_11506 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Size of the accretion disc in the recurrent nova T CrB Zamanov, R. K. Stoyanov, K. A. Marchev, V. Minev, M. Marchev, D. Moyseev, M. Marti, J. Bode, M. F. Konstantinova-Antova, R. Stefanov, S. Solar and Stellar Astrophysics 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 $R_{disc} = 89 \pm 19$ 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. |
| title | Size of the accretion disc in the recurrent nova T CrB |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2405.11506 |