太阳黑子中Evershed流的时间演化。I. Evershed云的观测特征
Temporal evolution of the Evershed flow in sunspots. I. Observational characterization of Evershed clouds
摘要：
[摘要]光球Evershed流的磁性和运动学性质相对较为人所知，但我们仍然远远没有完全了解其性质。流动随时间的演变，这主要是由于出现的速度包称为Evershed云（EC），可以提供信息，以进一步限制其起源。在这里，我们进行了详细的分析的演变Evershed流通过研究EC的属性。在这第一篇论文中，我们确定的大小，适当的运动，在半影的位置，和频率的出现EC，以及他们的典型的多普勒速度，线和圆偏振信号，斯托克斯V面积不对称性，和连续强度。高节奏，高分辨率，全矢量光谱偏振测量在可见光和红外线被用来获得这些参数。我们发现，EC出现在半影的中间，并propage沿大的线偏振信号和增强的Evershed流的细丝向外。在不同的细丝中，EC出现的频率在15和40分钟之间变化。EC表现出最大的多普勒速度和线圆偏振比的整个半影。此外，在大气深处形成的线显示出更大的多普勒速度，与“静止”的埃弗谢德流的方式大致相同。根据我们的观察，EC可以分为两类：I型EC，消失在外半影，和II型EC，穿过外半影边界，进入太阳黑子护城河。大多数观察到的EC属于I型。平均而言，II型EC可以检测到的速度结构以外的现场只有约14分钟。他们的自行车在护城河显着减少相对于他们在半影。
英文摘要：
[Abridged] The magnetic and kinematic properties of the photospheric Evershed flow are relatively well known, but we are still far from a complete understanding of its nature. The evolution of the flow with time, which is mainly due to appearance of velocity packets called Evershed clouds (ECs), may provide information to further constrain its origin. Here we undertake a detailed analysis of the evolution of the Evershed flow by studying the properties of ECs. In this first paper we determine the sizes, proper motions, location in the penumbra, and frequency of appearance of ECs, as well as their typical Doppler velocities, linear and circular polarization signals, Stokes V area asymmetries, and continuum intensities. High-cadence, high-resolution, full vector spectropolarimetric measurements in visible and infrared lines are used to derive these parameters. We find that ECs appear in the mid penumbra and propage outward along filaments with large linear polarization signals and enhanced Evershed flows. The frequency of appearance of ECs varies between 15 and 40 minutes in different filaments. ECs exhibit the largest Doppler velocities and linear-to-circular polarization ratios of the whole penumbra. In addition, lines formed deeper in the atmosphere show larger Doppler velocities, much in the same way as the ''quiescent'' Evershed flow. According to our observations, ECs can be classified in two groups: type I ECs, which vanish in the outer penumbra, and type II ECs, which cross the outer penumbral boundary and enter the sunspot moat. Most of the observed ECs belong to type I. On average, type II ECs can be detected as velocity structures outside of the spot for only about 14 min. Their proper motions in the moat are significantly reduced with respect to the ones they had in the penumbra.
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