arXiv 1602.041542016-02-12astro-ph.SR

用HMI观测太阳黑子大小双极区的倾角和足点分离

Tilt Angle and Footpoint Separation of Small and Large Bipolar Sunspot Regions Observed with HMI

Bruce H. McClintock, Aimee A. Norton

备注：: 16 pages, 1 table, 4 figures
发表信息：: ApJ, 818, 7 (2016)
DOI：: 10.3847/0004-637X/818/1/7

摘要：

我们调查了双极太阳黑子区域，以及在出现和衰退期间倾斜角和足迹分离是如何变化的。太阳动力学观测台上的日震和磁成像仪以高于历史记录的节奏收集数据，并允许对区域的生命周期进行详细分析。我们采样的本影倾斜角，足点分离，和本影面积的235双极太阳黑子地区的日震和磁成像仪-德布勒森数据（HMIDD）与每小时的节奏。我们使用本影面积达到峰值的时间作为零时间来区分每个区域的出现和衰退期，并且我们将对倾斜和分离行为随时间的分析限制在零时间的+/-96小时内。矩形演化对于具有小（~30 MSH）、中等（~50 MSH）和大（~110 MSH）最大阴影区域的区域是明显不同的，45和90 MSH是分离组的有用划分。在峰值阴影区域，我们确定了小（7.6度）、中等（5.9度）和大（9.3度）区域的中位倾斜角。在+/-48小时内的时间的峰值阴影区，大区域的倾斜角稳步增加，中型地区几乎是恒定的，和小区域显示出证据的负倾斜在出现。对于大约40至70 Mm的所有区域，足点分离的增长期发生在72小时内。最小的双极（< 9 MSH）是离群值，因为它们不遵守乔伊定律，并且具有小得多的足点分离。我们证实了Munoz-Jaramillo等人（2015）的结果，即太阳黑子似乎是两个不同的种群。

英文摘要：

We investigate bipolar sunspot regions and how tilt angle and footpoint separation vary during emergence and decay. The Helioseismic and Magnetic Imager on board the Solar Dynamic Observatory collects data at a higher cadence than historical records and allows for a detailed analysis of regions over their lifetimes. We sample the umbral tilt angle, footpoint separation, and umbral area of 235 bipolar sunspot regions in Helioseismic and Magnetic Imager - Debrecen Data (HMIDD) with an hourly cadence. We use the time when the umbral area peaks as time zero to distinguish between the emergence and decay periods of each region and we limit our analysis of tilt and separation behavior over time to within +/-96 hours of time zero. Tilt angle evolution is distinctly different for regions with small (~30 MSH), midsize (~50 MSH), and large (~110 MSH) maximum umbral areas, with 45 and 90 MSH being useful divisions in separating the groups. At the peak umbral area, we determine median tilt angles for small (7.6 degrees), midsize (5.9 degrees) and large (9.3 degrees) regions. Within +/-48 hours of the time of peak umbral area, large regions steadily increase in tilt angle, midsize regions are nearly constant, and small regions show evidence of negative tilt during emergence. A period of growth in footpoint separation occurs over a 72-hr period for all of the regions from roughly 40 to 70 Mm. The smallest bipoles (< 9 MSH) are outliers in that they do not obey Joy's law and have a much smaller footpoint separation. We confirm Munoz-Jaramillo et al. (2015) results that the sunspots appear to be two distinct populations.

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