论文标题
磁性明亮点（MBP）中色球振荡周期的特征
Characteristics of Chromospheric Oscillation Periods in Magnetic Bright Points (MBPs)
论文作者
论文摘要
在这项研究中，研究了MG II K线强度，亮度温度和多普勒速度（MBP）获得的振荡周期。为此，将观察到较高色球圈和过渡区域（TR）的界面区域成像光谱仪（IRIS）的数据与通过太阳能动力学观测站（SDO）获得的成像和磁力图数据进行了分析。在将SI IV 1403 A SLIT JAW图像（SJIS）与来自Heliospheric和Magement Imagemer（HMI）的磁化图信息（HMI）相结合时，发现了Mbps。在MG II K（2796 A和10,000 K）的共振线上进行振荡期的MG II K（2796 A和10,000 K）的共振线进行了时机分析。最后，进行了功率谱分析以表征振荡，结果网络点具有典型的强度，温度和速度振荡周期约为300秒。互联网工作点的平均强度振荡周期约为180秒，平均温度振荡周期约为202，平均速度振荡周期约为202秒。此外，对一个BP进行了详细分析，该BP证明了500秒的强度振荡周期，显然与色层/光晶结构中通常在其他地方发现的常见的3或5分钟振荡无关。
In this investigation oscillation periods in Mg II k line intensity, brightness temperature, and Doppler velocity obtained above Magnetic Bright Points (MBPs) are investigated. For that purpose, data from the Interface Region Imaging Spectrometer (IRIS) observing the higher chromosphere and transition region (TR) were analysed together with imaging and magnetogram data obtained by Solar Dynamics Observatory (SDO). The MBPs were identified in combining Si IV 1403 A Slit Jaw Images (SJIs) with the magnetogram information from the Heliospheric and Magnetic Imager (HMI). A time-slice analysis followed by a wavelet inspection were carried out on the Mg II k (2796 A and 10,000 K) resonance lines for the detection of the oscillation period. Finally, a power spectrum analysis was performed to characterise the oscillations with the result that network points feature a typical intensity, temperature, and velocity oscillation period of about 300 seconds; The internetwork points have a mean intensity oscillation period of about 180 seconds, mean temperature oscillation period of about 202, and mean velocity oscillation period of about 202 seconds. In addition, one BP was analysed in detail, which demonstrates intensity oscillation periods with a value of 500 seconds, obviously not related to the common 3- or 5-minute oscillations found typically elsewhere in chromospheric/photospheric structures.
