关于光斑亮度的起源
On the origin of facular brightness
摘要：
本文研究了日冕线核亮度与光球磁场的强度和倾角，以及与太阳盘中心光斑区的对流和波动参数的关系。我们使用德国真空塔望远镜获得的三个同步数据集（特内里费岛泰德天文台）：（1）用TESOS仪器记录的BaII 4554 A谱线的光谱，以测量穿过光球层直到最低温度的强度和速度变化;（2）FeI 1.56 $μ$ m谱线的分光偏振数据（与仪器TIP II注册），以测量光球磁场;（3）在CaIIH中的滤波图，提供有关色球层亮度波动的信息。结果表明，在光斑的CaIIH亮度强烈地依赖于功率的波周期在5分钟的范围内，向上传播，也对相移之间的速度振荡在底部光球和周围的温度最低的高度，从BaII线测量。CaIIH亮度在温度和速度振荡之间的相移在0-100度范围内的位置处最大。对流运动对CaIIH的亮度有间接影响。也就是说，对流速度的振幅越大，它们改变运动方向的高度越大，光斑越亮。总而言之，我们的结果导致的结论，光斑区域出现明亮，不仅是因为威尔逊抑郁症的磁结构，但也由于真正的加热。
英文摘要：
This paper studies the dependence of the CaIIH line core brightness on the strength and inclination of photospheric magnetic field, and on the parameters of convective and wave motions in a facular region at the solar disc center. We use three simultaneous datasets obtained at the German Vacuum Tower Telescope (Observatorio del Teide, Tenerife): (1) spectra of BaII 4554 A line registered with the instrument TESOS to measure the variations of intensity and velocity through the photosphere up to the temperature minimum; (2) spectropolarimetric data in FeI 1.56 $μ$m lines (registered with the instrument TIP II) to measure photospheric magnetic fields; (3) filtergrams in CaIIH that give information about brightness fluctuations in the chromosphere. The results show that the CaIIH brightness in the facula strongly depends on the power of waves with periods in the 5-min range, that propagate upwards, and also on the phase shift between velocity oscillations at the bottom photosphere and around the temperature minimum height, measured from BaII line. The CaIIH brightness is maximum at locations where the phase shift between temperature and velocity oscillations lies within 0-100 degrees. There is an indirect influence of convective motions on the CaIIH brightness. Namely, the higher is the amplitude of convective velocities and the larger is the height where they change their direction of motion, the brighter is the facula. Altogether, our results lead to conclusions that facular regions appear bright not only because of the Wilson depression in magnetic structures, but also due to real heating.
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。
