Afterglow Light Curves of Nonrelativistic Ejecta Mass in a Stratified Circumstellar Medium
Afterglow Light Curves of Nonrelativistic Ejecta Mass in a Stratified Circumstellar Medium
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DOI：
10.3847/1538-4357/abcaf6
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发表时间：
2020-06
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通讯作者：
N. Fraija;B. B. Kamenetskaia-B.;M. Dainotti;R. Duran;A. G. G'amez;S. Dichiara;S. PedreiraA.C.CaliguladoE.
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作者：
N. Fraija;B. B. Kamenetskaia-B.;M. Dainotti;R. Duran;A. G. G'amez;S. Dichiara;S. PedreiraA.C.CaliguladoE.
我们给出了在密度分布为n（r）<$r−k（k = 0，1，1.5，2和2.5）的分层星周介质中非相对论性喷出物质量减速产生的余辉光变曲线。一旦抛射物质以E（>β）<$β−α（其中β是抛射速度）参数化的等效动能发射并传播到周围的星周介质中，它首先以恒定速度移动（自由滑行阶段），然后减速（Sedov-Taylor展开）。我们提出了预测的同步和同步自康普顿光变曲线在自由滑行阶段和随后的Sedov-Taylor展开。在特定的情况下，我们显示了相应的光变曲线的减速过程中发射的两个紧凑的物体和垂死的大质量恒星的核心崩溃，这将有助于在不同的时间尺度，频率和强度的合并的几个喷出物质量具有不同的速度。最后，使用多波长观测和上限收集的轨道卫星和地面望远镜的大运动，我们约束的参数空间的kilonova（KN）余辉在GW 170817和可能产生的KN余辉在S190814 bv。需要对合并后年份的时间尺度进行进一步观察，以得出更严格的限制。
We present the afterglow light curves produced by the deceleration of a nonrelativistic ejecta mass in a stratified circumstellar medium with a density profile n(r) ∝ r−k with k = 0, 1, 1.5, 2, and 2.5. Once the ejecta mass is launched with equivalent kinetic energy parameterized by E(>β) ∝ β−α (where β is the ejecta velocity) and propagates into the surrounding circumstellar medium, it first moves with constant velocity (the free-coasting phase), and later it decelerates (the Sedov–Taylor expansion). We present the predicted synchrotron and synchrotron self-Compton light curves during the free-coasting phase and the subsequent Sedov–Taylor expansion. In particular cases, we show the corresponding light curves generated by the deceleration of several ejecta masses with different velocities launched during the coalescence of binary compact objects and the core collapse of dying massive stars, which will contribute at distinct timescales, frequencies, and intensities. Finally, using the multiwavelength observations and upper limits collected by a large campaign of orbiting satellites and ground telescopes, we constrain the parameter space of both the kilonova (KN) afterglow in GW170817 and the possibly generated KN afterglow in S190814bv. Further observations on timescales of years post-merger are needed to derive tighter constraints.