Multiwavelength observations of multiple eruptions of the recurrent nova M31N 2008-12a

Judhajeet Basu*, M. Pavana, G. C. Anupama, Sudhanshu Barway, Kulinder Pal Singh, Vishwajeet Swain, Shubham Srivastav, Harsh Kumar, Varun Bhalerao, L. S. Sonith, G. Selvakumar

*Corresponding author for this work

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We report the optical, UV, and soft X-ray observations of the 2017–2022 eruptions of the recurrent nova M31N 2008-12a. We find a cusp feature in the r′ - and i′ -band light curves close to the peak, which could be related to jets. The geometry of the nova ejecta based on morpho-kinematic modeling of the Hα emission line indicates an extended jet-like bipolar structure. Spectral modeling indicates an ejecta mass of 10−7–10−8 M ⊙ during each eruption and an enhanced helium abundance. The supersoft source phase shows significant variability, which is anticorrelated to the UV emission, indicating a common origin. The variability could be due to the reformation of the accretion disk. We infer a steady decrease in the accretion rate over the years based on the intereruption recurrence period. A comparison of the accretion rate with different models on the MWD–Ṁ plane yields the mass of a CO white dwarf, powering the H-shell flashes every ∼1 yr, to be >1.36 M ⊙ and growing with time, making M31N 2008-12a a strong candidate for the single degenerate scenario of the Type Ia supernovae progenitor.
Original languageEnglish
Article number44
Number of pages20
JournalThe Astrophysical Journal
Issue number1
Early online date24 Apr 2024
Publication statusPublished - 01 May 2024


  • Andromeda Galaxy
  • Photometry
  • Recurrent novae
  • X-ray astronomy
  • Cataclysmic variable stars
  • Ultraviolet astronomy
  • Transient sources
  • Spectroscopy


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