A MODEL OF MIRA'S COMETARY HEAD/TAIL ENTERING THE LOCAL BUBBLE
A MODEL OF MIRA'S COMETARY HEAD/TAIL ENTERING THE LOCAL BUBBLE
复制标题
米拉彗星头/尾进入局部气泡的模型
DOI：
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发表时间：
2010
期刊：
影响因子：
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通讯作者：
F. De Colle
中科院分区：
文献类型：
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作者：
A. Esquivel;A. Raga;J. Cantó;A. Rodríguez;D. López;P. Velázquez;F. De Colle
我们将米拉周围的彗星结构建模为来自米拉 A 的渐近巨型分支星风与流环境的相互作用。我们的模拟引入了以下新元素：我们假设在稠密环境中进化 200 kyr 后，Mira 进入了局部气泡（低密度日冕气体）。当米拉进入气泡时，彗星的头部膨胀得相当快，而彗尾在>100 kyr的时间尺度内保持良好的准直。结果是一个宽头/窄尾结构，类似于观察到的米拉彗星的形态。模拟是使用我们新的自适应网格代码 Walicxe 进行的，该代码有详细描述。
We model the cometary structure around Mira as the interaction of an asymptotic giant branch stellar wind from Mira A with a streaming environment. Our simulations introduce the following new element: we assume that after 200 kyr of evolution in a dense environment, Mira entered the Local Bubble (low-density coronal gas). As Mira enters the bubble, the head of the comet expands quite rapidly, while the tail remains well collimated for a >100 kyr timescale. The result is a broad-head/narrow-tail structure that resembles the observed morphology of Mira's comet. The simulations were carried out with our new adaptive grid code Walicxe, which is described in detail.