论文标题
内气球内磁场光谱演化
Magnetic field spectral evolution in the inner heliosphere
论文作者
论文摘要
Parker太阳能探针和太阳轨道数据用于研究磁性湍流在$ 0.06〜 \ Lessim r〜 \ Lessim 1 $ au之间的径向演变。将频谱作为比例的函数研究，并标准化为离子惯性尺度$ d_ {i} $。在太阳附近，惯性范围仅限于狭窄范围，并显示出$α__{b} = -3/2 $的功率法指数，独立于等离子体参数。惯性范围随距离而生长，逐渐扩展到较大的空间尺度，同时朝着$α_{b} = -5/3 $缩放缩放。可以观察到，与高度alfvénic间隔相比，磁能过量和低藻类含量的间隔显着陡峭，而距离保持近似缩放。较慢的风流中陡峭光谱的发生可能归因于观察到的太阳风速和藻类之间的正相关。
Parker Solar Probe and Solar Orbiter data are used to investigate the radial evolution of magnetic turbulence between $0.06 ~ \lesssim R ~\lesssim 1$ au. The spectrum is studied as a function of scale, normalized to the ion inertial scale $d_{i}$. In the vicinity of the Sun, the inertial range is limited to a narrow range of scales and exhibits a power-law exponent of, $α_{B} = -3/2$, independent of plasma parameters. The inertial range grows with distance, progressively extending to larger spatial scales, while steepening towards a $α_{B} =-5/3$ scaling. It is observed that spectra for intervals with large magnetic energy excesses and low Alfvénic content steepen significantly with distance, in contrast to highly Alfvénic intervals that retain their near-Sun scaling. The occurrence of steeper spectra in slower wind streams may be attributed to the observed positive correlation between solar wind speed and Alfvénicity.
