Issue |
A&A
Volume 689, September 2024
|
|
---|---|---|
Article Number | A60 | |
Number of page(s) | 7 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/202449919 | |
Published online | 30 August 2024 |
Primary and secondary source of energy in the superluminous supernova 2018ibb
1
Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany
2
GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany
3
National Research Center, Kurchatov Institute, pl. Kurchatova 1, Moscow 123182, Russia
4
Lebedev Physical Institute, Russian Academy of Sciences, 53 Leninsky Avenue, Moscow 119991, Russia
5
Space Research Institute (IKI), Profsoyuznaya 84/32, Moscow 117997, Russia
6
M.V. Lomonosov Moscow State University, Sternberg Astronomical Institute, 119234 Moscow, Russia
7
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
Received:
9
March
2024
Accepted:
30
May
2024
We examined a possible pair-instability origin for the superluminous supernova 2018ibb. As the base model, we used a non-rotating stellar model with an initial mass of 250 M⊙ at about 1/15 solar metallicity. We considered three versions of the model as input for radiative transfer simulations done with the STELLA and ARTIS codes: with 25 M⊙ of 56Ni, with 34 M⊙ of 56Ni, and a chemically mixed case with 34 M⊙ of 56Ni. We present light curves and spectra in comparison to the observed data of SN 2018ibb, and conclude that the pair-instability supernova model with 34 M⊙ of 56Ni explains the broadband light curves reasonably well between −100 and 250 days around the peak. Our synthetic spectra have many similarities with the observed spectra. The luminosity excess in the light curves and the blue-flux excess in the spectra can be explained by an additional energy source, which may be an interaction of the supernova ejecta with circumstellar matter. We discuss possible mechanisms that could have caused the circumstellar matter to be ejected in the decades before the pair-instability explosion.
Key words: radiative transfer / circumstellar matter / stars: massive / supernovae: general / supernovae: individual: 2018ibb
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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