Bipolar Magnetic Regions determined from Kitt Peak Vacuum Telescope Magnetograms

Citation and Acknowledgements Please cite both this database, the papers describing it, as well as adding the following acknowledgement: \"Bipolar magnetic regions determined from KPVT full disk magnetograms were downloaded from the solar dynamo dataverse (https://dataverse.harvard.edu/dataverse/solardynamo), maintained by Andrés Muñoz-Jaramillo.\" Database citation format is shown at the top of this page, underneath the database title. It can be downloaded in a variety of formats directly from this page The papers describing this database are N. R. Sheeley, Jr., C. R. DeVore, and J. P. Boris, Simulations of the mean solar magnetic field during sunspot cycle 21, Solar Physics 98, 219, (1985). http://adsabs.harvard.edu/abs/1985SoPh...98..219S N. R. Sheeley, Jr. and Y-M Wang, Average properties of bipolar magnetic regions during sunspot cycle 21, Solar Physics 124, 81, (1989). http://adsabs.harvard.edu/abs/1989SoPh..124...81W Main Limitations The main limitations of these data are: Only the magnetic flux of the largest polarity is logged, assuming that the bipole is in perfect balance. The darkening of umbrae leads to an underestimation of the magnetic field strength by the KPVT-512. It is possible that flux is underestimated for the largest regions. Lower sensitivity is not constant during the survey so more small objects are logged towards the end than at the beginning. Description Bipolar Mangetic Regions (BMR) determined from Kitt Peak Vacuum Telescope (KPVT) Magnetograms. Detection of each BMR was performed manually by Neil Sheeley, Jr. using printed full disk magnetograms. Each BMR is identified uniquely from the moment of disk appearance to disappearance (either by decay, merging, or rotation). Returns after a full rotation are counted as new structures. Each of BMR is logged only once in the database at the point of maximum development. Columns are as follows: Date of maximum development. Hour of maximum development. Flux of leading polarity (1021 Mx). Latitude of leading polarity centroid. Longitude of leading polarity centroid. Latitude of trailing polarity centroid. Longitude of trailing polarity centroid.

引用与致谢
请同时引用本数据库及其相关研究论文，并添加以下致谢内容："从基特峰真空望远镜（KPVT）全日面磁图提取的双极磁区数据下载自太阳动力学数据文库（solar dynamo dataverse，https://dataverse.harvard.edu/dataverse/solardynamo），该数据文库由Andrés Muñoz-Jaramillo维护。" 数据库引用格式详见本页面标题下方的顶部区域。用户可直接从本页面以多种格式下载本数据集。本数据集相关研究论文包括：N. R. Sheeley, Jr.、C. R. DeVore 与 J. P. Boris，《第21个太阳黑子周期间太阳平均磁场的模拟》，《Solar Physics》98, 219 (1985)，链接：http://adsabs.harvard.edu/abs/1985SoPh...98..219S；N. R. Sheeley, Jr. 与 Y-M Wang，《第21个太阳黑子周期间双极磁区的平均特性》，《Solar Physics》124, 81 (1989)，链接：http://adsabs.harvard.edu/abs/1989SoPh..124...81W。

主要局限性
本数据集存在以下主要局限性：1. 仅记录双极磁区中极性更强一侧的磁通量，假设双极结构完全平衡；2. 本影区域的暗化效应会导致基特峰真空望远镜（KPVT）-512对磁场强度的测量结果偏低；3. 大型磁区的磁通量可能存在低估情况；4. 本次观测的灵敏度并非恒定，观测后期记录的小尺度磁区数量多于观测初期。

数据集说明
本数据集包含从基特峰真空望远镜（Kitt Peak Vacuum Telescope, KPVT）磁图中提取的双极磁区（Bipolar Magnetic Regions, BMR）。每个双极磁区均由Neil Sheeley, Jr.通过打印的全日面磁图手动识别。每个双极磁区从其在日面出现至消失（通过衰减、合并或旋转消失）的全过程均被唯一标识；若某磁区经过完整太阳自转周期后再次出现，则将其视为新的结构。本数据库仅在每个双极磁区达到最大发展阶段时对其进行一次记录。数据集各字段说明如下：1. 最大发展阶段日期；2. 最大发展阶段时刻（小时）；3. 前导极性磁通量（单位：10²¹ 麦克斯韦，Mx）；4. 前导极性质心纬度；5. 前导极性质心经度；6. 后随极性质心纬度；7. 后随极性质心经度。