论文标题
分层的偶然介质中非相关射流质量的余辉光曲线
Afterglow light curves of the non-relativistic ejecta mass in a stratified circumstellar medium
论文作者
论文摘要
我们介绍了通过分层的间隔介质在具有密度型材$ n（r）\ propto r^{ - k} $的分层室内介质中的非相关弹射质量减速而产生的余波光曲线，$ k = 0 $，$ 1 $，$ 1 $，$ 1 $，$ 1.5 $，$ 2 $，$ 2 $和$ 2.5 $和$ 2.5 $。一旦以$ e（>β）\ proptoβ^{ - α} $参数为参数的等效动能发射（其中beta是beta是弹射速度），并以恒定的速度移动（自由构成的相位）（自由构成的相位），并在perseelians contecivor contecivor（persecriation conteciriation conteciriation）（betaine decover）（betaine decover）（betaine decover）（betera），它首先传播到周围的室内介质中，并扩展了contecianter contelianter（persecriant contecirions and Itcorvor）。我们介绍了自由播种阶段期间预测的同步加速器和同步体康普顿光曲线，以及随后的塞多夫 - 泰勒膨胀。在特定情况下，我们显示了通过在二元紧凑型物体合并期间发射的几个喷射质量的减速以及垂死的巨大恒星的核心散射产生的相应光曲线，这些曲线将在不同的时间表，频率，频率和强度下造成巨大的巨大恒星。最后，使用大型轨道卫星和地面望远镜收集的多波长观测和上限，我们限制了GW170817中的KN余辉的参数空间，以及在S190814BV中可能生成的KN浮力。需要进一步观察合并后年的时间尺度，以得出更严格的限制。
We present the afterglow light curves produced by the deceleration of the non-relativistic ejecta mass in a stratified circumstellar medium with a density profile $n(r)\propto r^{-k}$ with $k=0$, $1$, $1.5$, $2$ and $2.5$. Once the ejecta mass is launched with equivalent kinetic energy parametrized by $E(>β)\propto β^{-α}$ (where beta 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 multi-wavelength observations and upper limits collected by a large campaign of orbiting satellites and ground telescopes, we constrain the parameter space of both the 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.
