Multi-wavelength observations of multiple eruptions of the recurrent nova M31N 2008-12a
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| Main Authors: | , , , , , , , , , , |
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| Format: | Preprint |
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2023
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| _version_ | 1866913390968963072 |
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| author | Basu, Judhajeet Pavana, M. Anupama, G. C. Barway, Sudhanshu Singh, Kulinder Pal Swain, Vishwajeet Srivastav, Shubham Kumar, Harsh Bhalero, Varun Sonith, L. S. Selvakumar, G. |
| author_facet | Basu, Judhajeet Pavana, M. Anupama, G. C. Barway, Sudhanshu Singh, Kulinder Pal Swain, Vishwajeet Srivastav, Shubham Kumar, Harsh Bhalero, Varun Sonith, L. S. Selvakumar, G. |
| contents | We report the optical, UV, and soft X-ray observations of the $2017-2022$ eruptions of the recurrent nova M31N 2008-12a. We infer a steady decrease in the accretion rate over the years based on the inter-eruption recurrence period. We find a ``cusp'' feature in the $r'$ and $i'$ band light curves close to the peak, which could be associated to jets. Spectral modelling indicates a mass ejection of 10$^{-7}$ to 10$^{-8}$ M$_{\odot}$ during each eruption, and an enhanced Helium abundance of He/He$_{\odot}$ $\approx$ 3. The super-soft source (SSS) phase shows significant variability, which is anti-correlated to the UV emission, indicating a common origin. The variability could be due to the reformation of the accretion disk. A comparison of the accretion rate with different models on the $\rm M_{WD}$$-\dot{M}$ plane yields the mass of a CO WD, powering the ``H-shell flashes'' every $\sim$ 1 year to be $>1.36$ M$_{\odot}$ and growing with time, making M31N 2008-12a a strong candidate for the single degenerate scenario of Type Ia supernovae progenitor. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2310_06586 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Multi-wavelength observations of multiple eruptions of the recurrent nova M31N 2008-12a Basu, Judhajeet Pavana, M. Anupama, G. C. Barway, Sudhanshu Singh, Kulinder Pal Swain, Vishwajeet Srivastav, Shubham Kumar, Harsh Bhalero, Varun Sonith, L. S. Selvakumar, G. High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We report the optical, UV, and soft X-ray observations of the $2017-2022$ eruptions of the recurrent nova M31N 2008-12a. We infer a steady decrease in the accretion rate over the years based on the inter-eruption recurrence period. We find a ``cusp'' feature in the $r'$ and $i'$ band light curves close to the peak, which could be associated to jets. Spectral modelling indicates a mass ejection of 10$^{-7}$ to 10$^{-8}$ M$_{\odot}$ during each eruption, and an enhanced Helium abundance of He/He$_{\odot}$ $\approx$ 3. The super-soft source (SSS) phase shows significant variability, which is anti-correlated to the UV emission, indicating a common origin. The variability could be due to the reformation of the accretion disk. A comparison of the accretion rate with different models on the $\rm M_{WD}$$-\dot{M}$ plane yields the mass of a CO WD, powering the ``H-shell flashes'' every $\sim$ 1 year to be $>1.36$ M$_{\odot}$ and growing with time, making M31N 2008-12a a strong candidate for the single degenerate scenario of Type Ia supernovae progenitor. |
| title | Multi-wavelength observations of multiple eruptions of the recurrent nova M31N 2008-12a |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2310.06586 |