基于范艾伦卫星观测下太阳风动压对嘶声波分布的影响
doi: 10.11728/cjss2024.06.2024-yg26 cstr: 32142.14.cjss.2024-yg26
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袁安 男, 1998年8月出生于江西省新余市, 现为南昌大学空间科学与技术研究院博士研究生, 主要研究方向为磁层中哨声波的波粒相互作用. E-mail: yuanan@email.ncu.edu.cn -
李海梦 男, 1989年2月出生于山东聊城, 现为南昌大学空间科学与技术研究院副教授, 主要研究方向为内磁层中的动理学过程, 磁层–低电离层耦合研究, 电波传播, 深度学习与人工智能等. E-mail: lihaimeng@ncu.edu.cn
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Influence of Solar Wind Dynamic Pressure on Hiss Distribution Based on Van Allen Probe Observations
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摘要: 哨声波作为常见的等离子体波动, 对于磁层内能量电子的加速和损失起着重要作用. 已有统计研究表明, 地磁活动对哨声波的分布具有显著影响, 但是关于太阳风活动对其的影响多以事件报道为主. 本文使用范艾伦卫星5年的数据进行统计, 在排除亚暴注入的影响之后, 对等离子体层内嘶声在不同太阳风动压下的分布进行研究. 结果表明随着太阳风动压的增强, 30～200 Hz和200～500 Hz的嘶声振幅出现了减弱, 与太阳风动压的变化呈负相关. 与频率较低的嘶声相反, 500～1000 Hz以及1000～2500 Hz的嘶声振幅与太阳风动压的变化则是呈现正相关的趋势. 此外, 嘶声在磁纬上的分布没有明显的峰值, 这表明观测到的嘶声大部分都不是本地激发的. 而不同频段的嘶声对于太阳风动压的不同响应则可能是由于源区在太阳风动压增强时受到不同程度的影响所导致的. 研究嘶声对于太阳风变化的响应情况, 对于理解嘶声的起源与演化具有重要作用.Abstract: As a common plasma waves, whistler mode waves play a crucial role in the acceleration and scattering of energetic electrons in the magnetosphere. Numerous previous statistical studies have demonstrated that geomagnetic activities have a significant impact on the distribution of whistler waves. However, reports on the influence of solar wind activities on them are predominantly event-based. Five years of data from the Van Allen Probes were used for statistical analysis. After excluding the influence of substorm injections, the distribution of plasmaspheric hiss under different solar wind dynamic pressures were investigated. The results indicate that as the solar wind dynamic pressure intensifies, the amplitudes of hiss waves at 30～200 and 200～500 Hz exhibit a weakening trend and show a negative correlation with the change in solar wind dynamic pressure. In contrast to low frequency hiss, for hiss at 500～1000 Hz and 1000～2500 Hz, their amplitudes show a positive correlation trend with the change of solar wind. Additionally, there is no distinct peak in the distribution of hiss at magnetic latitudes, suggesting that most of the observed hiss is not locally excited. The different responses of hiss in different frequency bands to the solar wind dynamic pressure may be attributed to the fact that the source region is affected to varying degrees when the solar wind dynamic pressure increases. Studying the response of hiss to changes in the solar wind plays an important role in understanding the origin and evolution of hiss.
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Key words:
- Space plasma /
- Plasmaspheric hiss /
- Solar wind dynamic pressure /
- Magnetic longitude
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图 1 2013年2月28日06:30 UT－13:00 UT范艾伦探测器A的观测结果. (a)黑色曲线表示卫星观测的实际背景电子密度, 红色曲线表示由判定条件式(1)计算出来的密度. (b)卫星观测的磁场功率密度谱 (单位nT2· Hz–1). (c)卫星观测的波动极化谱. (d)观测的波法向角谱 [单位(°)]. (e)根据筛选条件判断之后挑选出来的嘶声波 (单位nT2· Hz–1). 在(b)～(e)中三条自上而下的实线、点虚线, 虚线分别表示1倍、0.5倍, 0.1倍的电子回旋频率
Figure 1. Observation results of the Van Allen Probe A from 06:30 UT to 13:00 UT on 28 February 2013. (a) The black curve represents the electron density observed by the satellite, and the red curve represents the density calculated by the judgment condition Eq.(1). (b) The magnetic spectral density observed by the satellite (unit nT2· Hz–1). (c) The wave polarization spectral observed by the satellite. (d) The observed wave normal angle [unit (°)]. (e) The hiss waves selected according to the selection conditions (unit nT2· Hz–1). (b)～(e) The solid lines, dotted-dashed lines, and dashed lines from top to bottom represent 1, 0.5, and 0.1 times the electron cyclotron frequency, respectively
图 2 (a)在AE' < 150 nT情况下所有采样点在L与λMLAT构成网格上的分布. (b)在同样条件下嘶声波平均振幅在L-λMLAT上的分布
Figure 2. (a) Distribution of all sampling points on the grid composed of L and λMLAT under the condition of AE' < 150 nT. (b) Distribution of the average amplitude hiss waves on L-λMLAT under the same condition
图 3 在不同强度的Psw下嘶声波平均振幅的分布. 每0.5L×2λMLAT格点范围内计算一次平均振幅. 右侧色条表示对应太阳风条件下每个格点中嘶声波振幅, 右下角小图代表对应的样本点数量
Figure 3. Distribution of the average amplitude of hiss waves under different intensities of Psw. The average amplitude is calculated within each bin of 0.5L×2λMLAT. The colorbar on the right side of the figure indicates the amplitude of hiss waves in each bin under the corresponding solar wind conditions. The small plot in the lower right corner of each panel represents the number of samples
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