论文标题
解释伽玛射线爆发的X射线余泽，散发性损失和毫秒磁铁
Interpreting the X-ray afterglows of gamma-ray bursts with radiative losses and millisecond magnetars
论文作者
论文摘要
毫秒磁铁的旋转能量已被调用，以解释X射线余辉的观测，这是短和长伽马射线爆发的显着部分。在这里，我们扩展了先前在文献中引入的模型，并通过任意制动指数将辐射损失与磁盘中央发动机的旋转旋转。将其与迅速发射尾巴的模型相结合，我们表明我们的模型可以更好地解释数据，而不是毫秒磁力模型，而没有辐射损失，或者仅通过真空偶极辐射旋转的模型就可以更好地解释数据。我们发现我们的模型预测了在某些伽马射线爆发中看到的X射线耀斑的子集。我们可以通过改变辐射效率并测量新生毫秒磁铁的制动指数来进一步解释X射线高原的多样性。我们将GRB061121的制动指数衡量为$ n = 4.85^{+0.11} _ { - 0.15} $，建议在这种伽马射线中诞生的毫秒毫秒爆发，这是通过重力波排放的主要旋转。
The spin-down energy of millisecond magnetars has been invoked to explain X-ray afterglow observations of a significant fraction of short and long gamma-ray bursts. Here, we extend models previously introduced in the literature, incorporating radiative losses with the spin down of a magnetar central engine through an arbitrary braking index. Combining this with a model for the tail of the prompt emission, we show that our model can better explain the data than millisecond-magnetar models without radiative losses or those that invoke spin down solely through vacuum dipole radiation. We find that our model predicts a subset of X-ray flares seen in some gamma-ray bursts. We can further explain the diversity of X-ray plateaus by altering the radiative efficiency and measure the braking index of newly-born millisecond magnetars. We measure the braking index of GRB061121 as $n=4.85^{+0.11}_{-0.15}$ suggesting the millisecond-magnetar born in this gamma-ray burst spins down predominantly through gravitational-wave emission.
