标题： 缺乏氢的光度超亮超新星，其光变曲线呈波浪状，由进动磁星提供能量 显示英文标题

标题： Hydrogen-poor Superluminous Supernovae with Bumpy Light Curves Powered by Precessing Magnetars

摘要： 最近的观测和统计研究显示，大量无氢超亮超新星（SLSNe-I）的光变曲线偏离了磁星驱动模型预测的平滑演化，而是在主峰之后表现出一个或多个凸起。然而，这些主峰后凸起的形成机制仍存在争议。此外，以往采用磁星驱动模型的研究通常假设固定的磁倾角，并忽略了磁星进动的影响。然而，最近的研究表明，大质量恒星坍缩过程中形成的新生磁星的进动会导致磁倾角随时间演变，从而影响磁偶极辐射。因此，本文将磁星进动的影响纳入磁星驱动模型，发展出进动磁星驱动模型。利用该模型，我们成功再现了6个具有主峰后凸起的代表性SLSNe-I的多波段光变曲线。此外，推导出的模型参数落在SLSNe-I的典型参数范围内。通过结合SLSNe-I和长伽马射线暴中的进动磁星，我们发现磁星的椭率与偶极磁场强度相关，这可能表明这两种现象有共同的起源。我们的工作为SLSNe-I主峰后凸起的起源提供了一种可能的解释，并为超新星爆炸中形成的新生磁星的早期进动提供了证据。 显示英文摘要

摘要： Recent observations and statistical studies have revealed that a significant fraction of hydrogen-poor superluminous supernovae (SLSNe-I) exhibit light curves that deviate from the smooth evolution predicted by the magnetar-powered model, instead showing one or more bumps after the primary peak. However, the formation mechanisms of these post-peak bumps remain a matter of debate. Furthermore, previous studies employing the magnetar-powered model have typically assumed a fixed magnetic inclination angle and neglected the effects of magnetar precession. However, recent research has shown that the precession of newborn magnetars forming during the collapse of massive stars causes the magnetic inclination angle to evolve over time, thereby influencing magnetic dipole radiation. In this paper, therefore, we incorporate the effects of magnetar precession into the magnetar-powered model to develop the precessing magnetar-powered model. Using this model, we successfully reproduce the multi-band light curves of 6 selected representative SLSNe-I with post-peak bumps. Moreover, the derived model parameters fall within the typical parameter range for SLSNe-I. By combining the precessing magnetars in SLSNe-I and long GRBs, we find that the ellipticity of magnetars is related to the dipole magnetic field strength, which may suggest a common origin for the two phenomena. Our work provides a potential explanation for the origin of post-peak bumps in SLSNe-I and offers evidence for the early precession of newborn magnetars formed in supernova explosions.