Applying an Automatic Image-Processing Method to Synoptic Observations
Applying an Automatic Image-Processing Method to Synoptic Observations
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DOI：
10.1007/s11207-013-0404-7
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发表时间：
2014-04
期刊：
影响因子：
2.8
通讯作者：
A. Tlatov;V. Vasil’eva;V. V. Makarova-V.;P. A. Otkidychev
中科院分区：
文献类型：
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作者：
A. Tlatov;V. Vasil’eva;V. V. Makarova-V.;P. A. Otkidychev
我们使用了自动图像处理方法来检测在基斯洛沃茨克太阳站观测到的白色光下的太阳活动特征。该技术可用于太阳黑子和活动区的自动或半自动探测。这种自动识别的结果与其他观测站提供的统计数据进行了验证，并显示出很高的检测精度。我们还提供了太阳黑子面积的参数，本影和光斑的观察，以及这些活动元素的磁通量，计算在基斯洛沃茨克太阳站，连同白光图像和magnetograms从迈克尔森多普勒成像仪板载太阳和日光层天文台（SOHO/MDI）。在第23太阳活动周期间，太阳黑子的本影面积与总面积之比为0.19。领先极性的太阳黑子面积大约是落后极性太阳黑子面积的2.5倍。
We used an automatic image-processing method to detect solar-activity features observed in white light at the Kislovodsk Solar Station. This technique was applied to automatically or semi-automatically detect sunspots and active regions. The results of this automated recognition were verified with statistical data available from other observatories and revealed a high detection accuracy. We also provide parameters of sunspot areas, of the umbra, and of faculae as observed in Solar Cycle 23 as well as the magnetic flux of these active elements, calculated at the Kislovodsk Solar Station, together with white-light images and magnetograms from theMichaelson Doppler Imageronboard theSolar and Heliospheric Observatory(SOHO/MDI). The ratio of umbral and total sunspot areas during Solar Cycle 23 is ≈ 0.19. The area of sunspots of the leading polarity was approximately 2.5 times the area of sunspots of the trailing polarity.