The solar wind exhibits scaling typical of intermittent turbulence in the statistics of in situ fluctuations in both the magnetic and velocity fields. Intriguingly, quantities not directly accessed by theories of ideal, incompressible, MHD turbulence, such as magnetic energy density, B-2, nevertheless show evidence of simple fractal (self-affine) statistical scaling. We apply a novel statistical technique which is a sensitive discriminator of fractality to the B-2 timeseries from WIND and ACE. We show that robust fractal behaviour occurs at solar maximum and determine the scaling exponents. The probability density function (PDF) of fluctuations at solar maximum and minimum are distinct. Power law tails are seen at maximum, and the PDF is reminiscent of a Levy flight. Citation: Hnat, B., S. C. Chapman, K. Kiyani, G. Rowlands, and N. W. Watkins (2007), On the fractal nature of the magnetic field energy density in the solar wind.
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机译：在磁场和速度场的原位波动统计中，太阳风均表现出间歇性湍流的典型标度。有趣的是，理想的，不可压缩的MHD湍流理论（例如磁能密度B-2）没有直接访问的量仍然显示出简单的分形（自仿射）统计定标的证据。我们将一种新颖的统计技术应用于分形从WIND和ACE的B-2时间序列中。我们表明鲁棒的分形行为发生在太阳最大值并确定比例指数。太阳最大和最小处的波动的概率密度函数（PDF）是不同的。幂律法尾部最多可见，PDF让人联想起征费飞行。引用：Hnat，B.，S. C. Chapman，K. Kiyani，G. Rowlands和N. W. Watkins（2007），论太阳风中磁场能量密度的分形性质。
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