تقرير
SN 2022jli: a type Ic supernova with periodic modulation of its light curve and an unusually long rise
| العنوان: | SN 2022jli: a type Ic supernova with periodic modulation of its light curve and an unusually long rise |
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| المؤلفون: | T., Moore, J., Smartt S., M., Nicholl, S., Srivastav, F., Stevance H., B., Jess D., T., Grant S. D., D., Fulton M., L., Rhodes, A., Sim S., R., Hirai, P., Podsiadlowski, P., Anderson J., C., Ashall, W., Bate, R., Fender, P., Gutierrez C., A., Howell D., E., Huber M., C., Inserra, G., Leloudas, G., Monard L. A., E., Muller-Bravo T., J., Shappee B., W., Smith K., G., Terreran, J., Tonry, A., Tucker M., R., Young D., A., Aamer, -W., Chen T., F., Ragosta, L., Galbany, M., Gromadzki, L., Harvey, P., Hoeflich, C., McCully, M., Newsome, P., Gonzalez E., C., Pellegrino, P., Ramsden, M., Perez-Torres, J., Ridley E., X., Sheng, J, Weston |
| سنة النشر: | 2023 |
| المجموعة: | Astrophysics |
| مصطلحات موضوعية: | Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics |
| الوصف: | We present multi-wavelength photometry and spectroscopy of SN 2022jli, an unprecedented Type Ic supernova discovered in the galaxy NGC 157 at a distance of $\approx$ 23 Mpc. The multi-band light curves reveal many remarkable characteristics. Peaking at a magnitude of $g=15.11\pm0.02$, the high-cadence photometry reveals 12.5$\pm0.2\ $day periodic undulations superimposed on the 200 day supernova decline. This periodicity is observed in the light curves from nine separate filter and instrument configurations with peak-to-peak amplitudes of $\simeq$ 0.1 mag. This is the first time that repeated periodic oscillations, over many cycles, have been detected in a supernova light curve. SN 2022jli also displays an extreme early excess which fades over $\approx$ 25 days followed by a rise to a peak luminosity of $L_{\rm opt} = 10^{42.1}$ erg s$^{-1}$. Although the exact explosion epoch is not constrained by data, the time from explosion to maximum light is $\gtrsim$ 59 days. The luminosity can be explained by a large ejecta mass ($M_{\rm ej}\approx12\pm6$M$_{\odot}$) powered by $^{56}$Ni but we find difficulty in quantitatively modelling the early excess with circumstellar interaction and cooling. Collision between the supernova ejecta and a binary companion is a possible source of this emission. We discuss the origin of the periodic variability in the light curve, including interaction of the SN ejecta with nested shells of circumstellar matter and neutron stars colliding with binary companions. Comment: Accepted in ApJL |
| نوع الوثيقة: | Working Paper |
| URL الوصول: | http://arxiv.org/abs/2309.12750 |
| رقم الأكسشن: | edsarx.2309.12750 |
| قاعدة البيانات: | arXiv |
| الوصف غير متاح. |