Kinematics of the v=1, J=1→0 SiO masers at 43 GHz towards TX Cam – a new 73-frame movie
Kinematics of the v=1, J=1→0 SiO masers at 43 GHz towards TX Cam – a new 73-frame movie
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DOI：
10.1111/j.1365-2966.2010.16716.x
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发表时间：
2010-07
影响因子：
4.8
通讯作者：
I. Gonidakis;P. Diamond;A. Kemball
中科院分区：
文献类型：
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作者：
I. Gonidakis;P. Diamond;A. Kemball
我们提出了一个新版本的电影的SiO脉泽周围的米拉变量TX凸轮。它由73帧（60个观测纪元）组成，数据涵盖了1997年5月24日至2000年5月21日之间几乎两个完整的恒星周期。使用甚长基线阵列每两周进行一次观测，之后每月进行一次观测。本文的目的是讨论星星在扩展大气中辐射的整体性质以及单个组分的运动学。还研究了冲击波的存在及其对气体形态和运动学的贡献，并与理论模型进行了比较。与第一个周期中观察到的主要膨胀相反，在第二个周期中观察到膨胀和收缩。脉泽变率与星星的脉动有关，而与光强无关。大多数已确定的单个组件遵循环的行为，但也有例外，具有更复杂的三维轨迹。
We present a new version of the movie of the SiO masers around the Mira variable TX Cam. It consists of 73 frames (60 observed epochs) with data covering almost two complete stellar cycles between 1997 May 24 and 2000 May 21. Observations were carried out using the Very Long Baseline Array in biweekly and later at monthly intervals. The purpose of this paper is to discuss the global properties of the emission in the extended atmosphere of the star as well as the kinematics of individual components. The existence of shock waves and their contribution to the morphology and the kinematics of the gas is also examined and compared with theoretical models. Contrary to the dominant expansion observed in the first cycle, both expansion and contraction are observed in the second cycle. The maser variability is correlated with the pulsation of the star but not with the optical intensity. Most of the individual components identified follow the behaviour of the ring, but there are exceptions with more complex three-dimensional trajectories.