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Increase of the Magnetic Flux From Polar Zones of the sun in the Last 120 Years

机译：近120年来来自太阳极区的磁通量增加

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Lockwood, Stamper, and Wild (1999) argued that the average strength of the magnetic field of the Sun has doubled in the last 100 years. They used an analysis of the geomagnetic index 〈aa〉. We calculated the area of polar zones of the Sun, A pz, occupied by unipolar magnetic field on Hα synoptic magnetic charts, following Makarov (1994), from 1878 to 2000. We found a gradual decrease of the annual minimum latitude of the high-latitude zone boundaries, θ2m, of the global magnetic field of the Sun at the minimum of activity from 53° in 1878 down to 38° in 1996, yielding an average decrease of 1.2° per cycle. Consequently the area of polar zones A pz of the Sun, occupied by unipolar magnetic field at the minimum activity, has risen by a factor of 2 during 1878–1996. This means that the behavior of the index 〈aa〉 and consequently the magnetic flux from the Sun may be explained by an increase of the area of polar caps with roughly the same value of the magnetic field in this period. The area of the unipolar magnetic field at the poles (A pz) may be used as a new index of magnetic activity of the Sun. We compared A pz with the 〈aa〉, the Wolf number 〈W〉 and 〈A〉* -index (Makarov and Tlatov, 2000). Correlations based on `11-year' averages are discussed. A temperature difference of about 1° between the Maunder Minimum and the present time was deduced. We have found that the highest latitude of the polar zone boundaries of the large-scale magnetic field during very low solar activity reaches about 60°, cf., the Maunder Minimum. It is supposed that the θ2m-latitude coincides with the latitude where ∂rω=0, with ω(r,θ) being the angular frequency of the solar rotation. The causes of the waxing and waning of the Sun's activity in conditions like Maunder Minimum are discussed.
机译：洛克伍德，斯坦珀和怀尔德（1999）认为，在过去100年中，太阳磁场的平均强度已经翻了一番。他们使用了对地磁指数的分析。根据Makarov（1994），从1878年到2000年，我们计算了Hα天气磁图上单极磁场占据的太阳极区A pz 的面积。我们发现年最小纬度逐渐减小太阳的高纬度区域边界的θ2m在最小活动度时从1878年的53°下降到1996年的38°，每个周期平均下降1.2°。因此，在1878年至1996年期间，以最小活动被单极磁场占据的太阳的极区A pz 的面积增加了2倍。这意味着指数的行为以及因此产生的来自太阳的磁通量可以用在此期间内具有大致相同磁场值的极帽面积增加来解释。极点处的单极磁场面积（A pz ）可以用作太阳磁活动的新指标。我们将A pz 与〈aa〉，沃尔夫数〈W〉和〈A〉 * -index进行了比较（Makarov和Tlatov，2000）。讨论了基于“ 11年”平均值的相关性。推断出Maunder Minimum与当前时间之间的温度差约为1°。我们已经发现，在极低的太阳活动期间，大型磁场的极区边界的最高纬度达到约60°，参见Maunder Minimum。假设θ2m纬度与∂rω= 0的纬度一致，其中ω（r，θ）为太阳旋转的角频率。讨论了在Maunder Minimum之类的条件下太阳活动蜡化和减弱的原因。

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  • 来源
    《Solar Physics》 |2002年第2期|383-399|共17页
  • 作者

    V.I. Makarov; A.G. Tlatov; D.K. Callebaut; V.N. Obridko;

  • 作者单位

    Pulkovo Astronomical Observatory;

    Pulkovo Astronomical Observatory;

    Physics Department UIA University of Antwerp;

    Ionosphere and Radio Wave Propagation (IZMIRAN) Institute of Terrestrial Magnetism;

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