Mira彗星头/尾进入局部气泡的模型
A model of Mira's cometary head/tail entering the Local Bubble
摘要：
我们模拟了米拉周围的彗星结构，作为来自米拉A的AGB风和流动环境的相互作用。我们的模拟引入了以下新的元素：我们假设米拉在稠密环境中进化了200 kyr后进入了局部气泡（低密度日冕气体）。当米拉进入气泡时，彗星的头部迅速膨胀，而尾部在100 kyr的时间尺度内保持良好的准直。结果是一个宽头/窄尾的结构，类似于观察到的米拉彗星的形态。我们的新的自适应网格代码WALICXE，这是详细描述进行了模拟。
英文摘要：
We model the cometary structure around Mira as the interaction of an AGB wind from Mira A, and 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.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
