Variable thermal energy injection from magnetar spin-down as a possible cause of stripped-envelope supernova light-curve bumps
| العنوان: | Variable thermal energy injection from magnetar spin-down as a possible cause of stripped-envelope supernova light-curve bumps |
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| المؤلفون: | Takashi J Moriya, Kohta Murase, Kazumi Kashiyama, Sergei I Blinnikov |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 513:6210-6218 |
| بيانات النشر: | Oxford University Press (OUP), 2022. |
| سنة النشر: | 2022 |
| مصطلحات موضوعية: | High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena |
| الوصف: | Luminosity evolution of some stripped-envelope supernovae such as Type I superluminous supernovae is difficult to be explained by the canonical 56Ni nuclear decay heating. A popular alternative heating source is rapid spin down of strongly-magnetized rapidly-rotating neutron stars (magnetars). Recent observations have indicated that Type I superluminous supernovae often have bumpy light curves with multiple luminosity peaks. The cause of bumpy light curves is unknown. In this study, we investigate the possibility that the light-curve bumps are caused by variations of the thermal energy injection from magnetar spin down. We find that a temporal increase in the thermal energy injection can lead to multiple luminosity peaks. The multiple luminosity peaks caused by the variable thermal energy injection is found to be accompanied by significant increase in photospheric temperature, and photospheric radii are not significantly changed. We show that the bumpy light curves of SN 2015bn and SN 2019stc can be reproduced by temporarily increasing magnetar spin-down energy input by a factor of 2-3 for 5-20 days. However, not all the light-curve bumps are accompanied by the clear photospheric temperature increase as predicted by our synthetic models. In particular, the secondary light-curve bump of SN 2019stc is accompanied by a temporal increase in photospheric radii rather than temperature, which is not seen in our synthetic models. We, therefore, conclude that not all the light-curve bumps observed in luminous supernovae are caused by the variable thermal energy injection from magnetar spin down and some bumps are likely caused by a different mechanism. 9 pages, 7 figures, accepted by Monthly Notices of the Royal Astronomical Society |
| تدمد: | 1365-2966 0035-8711 |
| الوصول الحر: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::7c84782f56a6b66d4a689b75af5644d7Test https://doi.org/10.1093/mnras/stac1352Test |
| حقوق: | OPEN |
| رقم الانضمام: | edsair.doi.dedup.....7c84782f56a6b66d4a689b75af5644d7 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 13652966 00358711 |
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