The behavior of sunspots is governed by the magnetic dynamo acting deep within the convection zone of the Sun. Therefore, knowledge of sunspot physical characteristics and how they evolve in time during a solar cycle can help to improve our understanding of the solar magnetic behavior. This work analyzes the physical characteristics of sunspots during the Solar Activity Cycle 23, detected using computer vision techniques. The main goal is to derive the relationships between sunspot properties. Images in visible light and magnetograms of the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory (SOHO) were used to detect sunspots and to extract their characteristics such as area, intensity (or temperature), and magnetic field magnitude. A total of 32,223 sunspots were analyzed, with longitudes between $-40^{\circ }$ and $40^{\circ }$ , throughout the entire Solar Cycle 23, from May 1996 through April 2008. These spots fell mainly into three categories. Most sunspots (85%) did not exhibit a well defined umbra, with average intensities larger than 0.657 relative to disk center, which corresponds to temperatures greater than 5200 K. A second group comprising less than 12% of the spots, was cooler (temperature less than 5200 K) and with more intense magnetic fields (2000 – 4000 G) and mostly presented a well defined umbra. Lastly, only 3% of the spots had large areas and strong magnetic fields with complex umbrae, but intermediate temperatures. The temporal behavior of sunspot physical characteristics throughout the 11 year cycle and the relationships between them were verified. Sunspot physical properties presented variations over time during Solar Cycle 23, such that larger, cooler sunspots with stronger magnetic fields occurred more frequently during periods of maximum activity. Linear correlations were found regarding the logarithm of the area and the intensity with extreme magnetic field, and of the temperature (or intensity) with the area; whereas a quadratic relation was found between magnetic field and temperature of spots.

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太阳活动周期 23 期间太阳黑子物理特征的相关性

太阳黑子的行为是由作用于太阳对流区深处的磁发电机控制的。因此，了解太阳黑子的物理特性以及它们在太阳周期中如何随时间演变，有助于提高我们对太阳磁行为的理解。这项工作分析了使用计算机视觉技术检测到的太阳活动周期 23 期间太阳黑子的物理特征。主要目标是推导出太阳黑子属性之间的关系。太阳和日球层天文台 (SOHO) 上的迈克尔逊多普勒成像仪 (MDI) 的可见光图像和磁力图用于探测太阳黑子并提取其特征，例如面积、强度（或温度）和磁场强度。总共分析了 32,223 个太阳黑子，经度在 $-40^{\circ }$ 和 $40^{\circ }$ 之间，贯穿整个太阳活动周期 23，从 1996 年 5 月到 2008 年 4 月。这些点主要分为三类。大多数太阳黑子 (85%) 没有表现出明确定义的本影，相对于圆盘中心的平均强度大于 0.657，这对应于高于 5200 K 的温度。包含少于 12% 的黑子的第二组较冷（温度小于 5200 K) 和更强烈的磁场 (2000 – 4000 G) 并且大多呈现出明确定义的本影。最后，只有 3% 的斑点面积大，磁场强，本影复杂，但温度适中。验证了整个 11 年周期中太阳黑子物理特征的时间行为及其之间的关系。在太阳活动周期 23 期间，太阳黑子的物理特性随时间发生变化，因此在最大活动期间，更大、更冷、磁场更强的太阳黑子更频繁地出现。发现区域与极端磁场强度的对数以及温度（或强度）与区域的对数呈线性相关；而磁场和点的温度之间存在二次关系。