论文标题
与Nustar的氢贫血超新星SN 2018HTI的硬X射线观测
Hard X-ray Observations of the Hydrogen-poor Superluminous Supernova SN 2018hti with NuSTAR
论文作者
论文摘要
一些贫苦的超小性超新星很可能由磁力中央发动机提供动力，使其比普通超新星的发光度更大。尽管从磁铁的旋转中预计会有很大的X射线通量，但仍将发现直接观察证据，从而导致“缺失的能量”问题。在这里，我们介绍了附近SN 2018HTI 2.4Y（休息框架）光峰后的Nustar观察结果。我们希望，到这个时候，弹射器在光子上已经变得比大约15kev的光子变得更薄。在超新星的位置未检测到$ f _ {\ rm {\ rm {10-30kev}} = 9.0 \ 9.0 \ times 10^{ - 14} $ erg cm $^{ - 2} $ s $ s $ s $^{ - 1} $，或$ 7.9 \ 7.9 \ $ 7.9 \ times 10^41} $ a的上限271MPC。这限制了从推定的旋转磁力旋转的降压亮度的比例为$ f _ {\ rm x} \ Lessim 36 $％在保守的情况下，在10-30kev范围内，$ f _ {\ rm x} \ rm x} \ rm x} \ lyssim在乐观案例中11 $％。
Some Hydrogen-poor superluminous supernovae are likely powered by a magnetar central engine, making their luminosity larger than common supernovae. Although a significant amount of X-ray flux is expected from the spin down of the magnetar, direct observational evidence is still to be found, giving rise to the "missing energy" problem. Here we present NuSTAR observations of nearby SN 2018hti 2.4y (rest frame) after its optical peak. We expect that, by this time, the ejecta have become optically thin for photons more energetic than about 15keV. No flux is detected at the position of the supernova down to $F_{\rm{10-30keV}} = 9.0\times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$, or an upper limit of $7.9 \times 10^{41}$ erg s$^{-1}$ at a distance of 271Mpc. This constrains the fraction of bolometric luminosity from the putative spinning down magnetar to be $f_{\rm X} \lesssim 36$% in the 10-30keV range in a conservative case, $f_{\rm X} \lesssim 11$% in an optimistic case.
