Magnetars are one of the potential power sources for some energetic supernova explosions such as type I superluminous supernovae (SLSNe I) and broad-lined type Ic supernovae (SNe Ic-BL). In order to explore the possible link between these two subclasses of supernovae (SNe), we study the effect of fallback accretion disk on magnetar evolution and magnetar-powered SNe. In this scenario, the interaction between a magnetar and a fallback accretion disk would accelerate the spin of the magnetar in the accretion regime but could result in substantial spin-down of the magnetars in the propeller regime. Thus, the initial rotation of the magnetar plays a less significant role in the spin evolution. Such a magnetar–disk interaction scenario can explain well the light curves of both SNe Ic-BL and SLSNe I, for which the observed differences are sensitive to the initial magnetic field of the magnetar and the fallback mass and timescale for the disk. Compared to the magnetars powering the SNe Ic-BL, those accounting for more luminous SNe usually maintain faster rotation and have relatively lower effective magnetic fields around peak time. In addition, the association between SLSNe I and long gamma-ray bursts, if observed in the future, could be explained in the context of a magnetar–disk system.

磁星是一些高能超新星爆炸的潜在动力源之一，例如 I 型超亮超新星 (SLSNe I) 和宽线 Ic 型超新星 (SNe Ic-BL)。为了探索这两个超新星 (SN) 亚类之间可能存在的联系，我们研究了回退吸积盘对磁星演化和磁星驱动的 SNe 的影响。在这种情况下，磁星和回退吸积盘之间的相互作用会加速吸积区中磁星的自旋，但可能导致螺旋桨区中磁星的自旋大幅下降。因此，磁星的初始旋转在自旋演化中扮演的角色不太重要。这样的磁盘相互作用场景可以很好地解释 SNe Ic-BL 和 SLSNe I 的光变曲线，观察到的差异对磁星的初始磁场和磁盘的回退质量和时间尺度敏感。与为超新星 Ic-BL 提供动力的磁星相比，那些拥有更明亮超新星的磁星通常保持更快的旋转，并且在峰值时间附近具有相对较低的有效磁场。此外，如果在未来观察到 SLSNe I 和长伽马射线暴之间的关联，可以在磁星盘系统的背景下进行解释。