Spica和PKS B1322-110年周期
Spica and the annual cycle of PKS B1322-110 scintillations
摘要：
PKS B1322-110是一个射电类星体，距离明亮的B星角宿一只有8.5'的角距离。它表现出一天内的变化，其通量密度在GHz频率归因于从等离子体不均匀性的湍流。我们已经用澳大利亚望远镜紧凑阵列跟踪了这个源的闪烁率一年多，记录了一个强大的年度周期，其中包括8月和12月的一次近乎停顿。该周期与高度各向异性的等离子体微观结构的散射是一致的，我们将我们的数据拟合到该模型中，以确定等离子体的运动学参数。由于PKS B1322-110的黄道纬度较低，等离子体微结构的取向受到很大限制。尽管如此，在每一个可能的方向上，我们的数据都挑选出了一个狭窄范围的相应速度分量，导致二维参数空间中的一维约束。约束区域与已发表的模型一致，其中散射材料与角宿一相关，并由围绕恒星径向取向的细丝组成。这个结果有1%的概率是偶然产生的。
英文摘要：
PKS B1322-110 is a radio quasar that is located only 8.5' in angular separation from the bright B star Spica. It exhibits intra-day variability in its flux density at GHz frequencies attributed to scintillations from plasma inhomogeneities. We have tracked the rate of scintillation of this source for over a year with the Australia Telescope Compact Array, recording a strong annual cycle that includes a near-standstill in August and another in December. The cycle is consistent with scattering by highly anisotropic plasma microstructure, and we fit our data to that model in order to determine the kinematic parameters of the plasma. Because of the low ecliptic latitude of PKS B1322-110, the orientation of the plasma microstructure is poorly constrained. Nonetheless at each possible orientation our data single out a narrow range of the corresponding velocity component, leading to a one-dimensional constraint in a two-dimensional parameter space. The constrained region is consistent with a published model in which the scattering material is associated with Spica and consists of filaments that are radially oriented around the star. This result has a 1% probability of arising by chance.
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