解释Mira尾部的发射机制差异及其在剪切界面中的演化
Reconciling the emission mechanism discrepancy in Mira's tail, and its evolution in an interface with shear
摘要：
GALEX对米拉AB双星系统的观测揭示了周围的结构，该结构已被成功地流体动力学解释为弓形激波和冲压压力剥离物质的尾部。即使是最初难以建模的窄尾，也被理解为米拉从温暖的中性介质进入热的低密度介质的影响，假设是局部气泡。然而，迄今为止还没有任何模型能够解释所观察到的扭结和相关的尾部一般曲率。我们测试的假设，在进入本地气泡，米拉是通过剪切流约1/3米拉自己的速度在一个角度为30度的米拉的自行车。这个假设重现了米拉尾巴的扭结性质，并预测尾部物质的再压缩和再加热到与冲击波中预测的密度和温度相同或更高的水平。这为FUV发射提供了热源，从而延长了FUV发射的寿命，这与对尾部年龄的其他估计一致。Mira的独特情况意味着在AGB恒星后面观察到其他FUV尾巴的可能性非常小。
英文摘要：
GALEX observations of the Mira AB binary system revealed a surrounding structure that has been successfully hydrodynamically interpreted as a bow shock and tail of ram-pressure-stripped material. Even the narrow tail, initially difficult to model, has been understood as the effect of the passage of Mira from a warm neutral medium into a hot, low-density medium, postulated to be the Local Bubble. However, no model to date has explained the observed kink and associated general curvature of the tail. We test the hypothesis that before entering the Local Bubble, Mira was travelling through a shear flow with approximately 1/3 Mira's own velocity at an angle of ~30degrees to Mira's proper motion. The hypothesis reproduces the kinked nature of Mira's tail and predicts recompression and reheating of the tail material to the same or greater levels of density and temperature predicted in the shock. This provides a heat source for the FUV emission, allowing for an extended lifetime of the FUV emission in line with other estimates of the age of the tail. The uniqueness of Mira's situation implies that the chances of observing other FUV tails behind AGB stars is highly unlikely.
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