超亮超新星光变特征和供能机制的统计分析

Light curve characteristics and energy sources of super-luminous supernovae:a statistical analysis

统计了91颗贫氢超亮超新星的光变特征,并结合3种供能模型进行了蒙特卡罗模拟,以探究实际观测对其能源机制的约束.结果显示:这些超亮超新星在g波段的平均峰值绝对星等为(-21.34±0.8),上升和下降时标分别分布在7~79和14~114 d,并呈现显著正相关;模拟结果表明磁星和相互作用机制都可能为大部分超亮超新星供能,在相互作用模型中,基于壳层分布假设的模拟结果与观测符合得更好.国内各大巡天项目(如CSST、司天工程)未来将探测到更多高红移超亮超新星,以期为相关科研人员深入了解宇宙中的恒星演化和爆炸过程提供重要数据.

Super-luminous supernovae have been studied intensively for nearly two decades.The high luminosity makes them of great significance for studying first-generation stars and early universe.However,the underlying energy mechanism remains unclear.In this study,91 hydrogen-poor super-luminous supernovae with wellsampled light curves were examined to extract their characteristics for statistical analysis.Markov Chain Monte Carlo simulations were carried out to reproduce these observables considering three power mechanisms.The constraints combining observations on their energy mechanism were systematically explored.The average peak absolute magnitude at g band was found to be(−21.34±0.8)mag,the rising and declining time scales were distributed in 7~79 and 14~114 d,where a strong correlation existed.Simulations indicated that both the magnetar and the interaction mechanism power.Under the interaction framework,the shell-like scenario is preferred based on comparison with observations.In the future,domestic telescopes and all-sky surveys(such as CSST and SiTian)will detect more super-luminous supernovae with high red shift,providing important information for a more comprehensive understanding of massive star evolution and explosions.