Gamma-Ray Bursts and Magnetar-forming Supernovae
Gamma-Ray Bursts and Magnetar-forming Supernovae
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伽马射线暴和形成磁星的超新星
DOI：
10.1007/s10509-011-0658-1
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发表时间：
2011
影响因子：
1.9
通讯作者：
M.
中科院分区：
文献类型：
--
作者：
Nomoto;K.;Maeda;K.;Tanaka;M.
长伽马射线暴（GRBs）与超新星（SNe）之间的联系已经通过观测得到证实。这些事件可以解释为一颗大质量恒星（M > 40M⊙）的核心迅速坍缩成黑洞（BH）。这些GRB-SNe的能量比典型的SNe大得多，因此这些SNe被称为超超新星（HNe）。SN 2006aj/GRB060218的情况有所不同：GRB微弱而柔和，被称为x射线闪光（XRF）；SN更暗，氧谱线也很弱。SN 2006aj的爆炸能量较小，喷射出的质量也较小。在我们的模型中，这颗祖恒星的质量比其他GRB-SNe （M ~ 20M⊙）要小，这表明形成的是一颗中子星（NS）而不是黑洞。如果新生的NS像磁星一样被强磁化并快速旋转，它可能会发射弱GRB或XRF。Ib型SN 2005bf奇特的光曲线也可能是由一颗磁星驱动的。2005bf的蓝移星云发射线表明，单极爆炸可能与新诞生的NS相关的持续吸积激波不稳定性（SASI）有关。
The connection between long Gamma Ray Bursts (GRBs) and Supernovae (SNe) have been established through the well observed cases. These events can be explained as the prompt collapse to a black hole (BH) of the core of a massive star (M≳40M⊙). The energies of these GRB-SNe were much larger than those of typical SNe, thus these SNe are called Hypernovae (HNe). The case of SN 2006aj/GRB060218 appears different: the GRB was weak and soft, being called an X-Ray Flash (XRF); the SN is dimmer and has very weak oxygen lines. The explosion energy of SN 2006aj was smaller, as was the ejected mass. In our model, the progenitor star had a smaller mass than other GRB-SNe (M∼20M⊙), suggesting that a neutron star (NS) rather than a BH was formed. If the nascent NS was strongly magnetized as a magnetar and rapidly spinning, it may launch a weak GRB or an XRF. The peculiar light curve of Type Ib SN 2005bf may also be powered by a magnetar. The blue-shifted nebular emission lines of 2005bf indicate the unipolar explosion possibly related to standing accretion shock instability (SASI) associated with a newly born NS.