dc.contributor.author |
Basu, Judhajeet |
|
dc.contributor.author |
Pavana, M |
|
dc.contributor.author |
Anupama, G. C |
|
dc.contributor.author |
Barway, Sudhanshu |
|
dc.contributor.author |
Singh, Kulinder Pal |
|
dc.contributor.author |
Swain, Vishwajeet |
|
dc.contributor.author |
Srivastav, Shubham |
|
dc.contributor.author |
Kumar, Harsh |
|
dc.contributor.author |
Bhalerao, Varun |
|
dc.contributor.author |
Sonith, L. S |
|
dc.contributor.author |
Selvakumar, G |
|
dc.date.accessioned |
2024-06-21T03:59:04Z |
|
dc.date.available |
2024-06-21T03:59:04Z |
|
dc.date.issued |
2024-05-01 |
|
dc.identifier.citation |
The Astrophysical Journal, Vol. 966, No. 1, 44 |
en_US |
dc.identifier.issn |
1538-4357 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/8479 |
|
dc.description |
Open Access. |
en_US |
dc.description |
Original content from this work may be used under the terms
of the Creative Commons Attribution 4.0 licence. Any further
distribution of this work must maintain attribution to the author(s) and the title
of the work, journal citation and DOI. |
|
dc.description.abstract |
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 Me 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 M M– WD plane yields the mass of a CO white dwarf, powering the H-shell flashes every ∼1 yr, to be >1.36 Me and growing with time, making M31N 2008-12a a strong candidate for the single degenerate scenario of the Type Ia supernovae progenitor. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
American Astronomical Society |
en_US |
dc.relation.uri |
https://doi.org/10.3847/1538-4357/ad2c8e |
|
dc.rights |
© 2024. The Author(s) |
|
dc.subject |
Recurrent novae |
en_US |
dc.subject |
Andromeda Galaxy |
en_US |
dc.subject |
Cataclysmic variable stars |
en_US |
dc.subject |
Transient sources |
en_US |
dc.subject |
Photometry |
en_US |
dc.subject |
Spectroscopy |
en_US |
dc.subject |
Ultraviolet astronomy |
en_US |
dc.subject |
X-ray astronomy |
en_US |
dc.title |
Multiwavelength Observations of Multiple Eruptions of the Recurrent Nova M31N 2008-12a |
en_US |
dc.type |
Article |
en_US |