MAGNETIC FIELD FLUCTUATIONS OBSERVED IN THE HELIOSHEATH AND INTERSTELLAR MAGNETIC FIELD BY VOYAGER 1 AT 115.7–124.9 AU DURING 2011–2013
MAGNETIC FIELD FLUCTUATIONS OBSERVED IN THE HELIOSHEATH AND INTERSTELLAR MAGNETIC FIELD BY VOYAGER 1 AT 115.7–124.9 AU DURING 2011–2013
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DOI：
10.1088/0004-637x/792/2/134
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发表时间：
2014-08
期刊：
影响因子：
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通讯作者：
L. Burlaga;N. Ness;V. Florinski;J. Heerikhuisen
中科院分区：
文献类型：
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作者：
L. Burlaga;N. Ness;V. Florinski;J. Heerikhuisen
我们讨论了航行者一号（V1）在2011.0至2012.3143（当它在遥远的日鞘内，平均磁场强度 <B> = 0.17 nT）和2012.6503至2013.5855（当它在遥远的日鞘内）期间（当它在星际等离子体 <B> = 0.47 nT)。在这两个区域中，波动主要是压缩波动，沿着平均 B（RTN 坐标中的 ≈T 方向）变化。在日鞘中，B 的压缩分量和横向分量的日标准偏差 (SD) 平均值为 <SDc> = 0.010 nT 和 <SDt> ⩽ 0.005 nT（这是测量的极限）。在遥远的日鞘中 <SDc>/<B> = 0.06，SD 的分布是偏斜且高度峰度的。星际磁场（ISMF）强度为B = 0.48 nT，但波动低于测量极限：<SDc> = 0.004 nT和<abs(SDt)> = 0.004 nT。这些星际标准差的分布具有与高斯噪声分布一致的偏度和峰度。我们还讨论了 V1 观测 ISMF 时，以 30 天为间隔，以 1 天为单位的 48 秒 B 平均值的波动情况。对于 B 的所有三个分量的波动，SD = 0.010 nT，这给出了 V1 观察到的尺度上 ISMF 波动的上限。该 SD 排除了在这些尺度上由拾取离子环不稳定性产生的电磁波动存在显着功率的可能性，这强烈限制了 IBEX 带的模型。
We discuss microscale fluctuations of the hour averages of the magnetic field B observed on a scale of one day by Voyager 1 (V1) from 2011.0 to 2012.3143 (when it was within the distant heliosheath, where the average magnetic field strength 〈B〉 = 0.17 nT) and during the interval from 2012.6503 to 2013.5855 (when it was within the interstellar plasma with 〈B〉 = 0.47 nT). In both regions, the fluctuations were primarily compressive fluctuations, varying along the average B (≈T direction in RTN coordinates). In the heliosheath, the average of the daily standard deviations (SDs) of the compressive and transverse components of B were 〈SDc〉 = 0.010 nT and 〈SDt〉 ⩽ 0.005 nT (which is the limit of the measurement). In the distant heliosheath 〈SDc〉/〈B〉 = 0.06, and the distributions of SD were skewed and highly kurtotic. The interstellar magnetic field (ISMF) strength was B = 0.48 nT, but the fluctuations were below the limit of measurement: 〈SDc〉 = 0.004 nT and 〈abs(SDt)〉 = 0.004 nT. The distributions of these interstellar SDs have skewness and kurtosis consistent with a Gaussian noise distribution. We also discuss the fluctuations of 48 s averages of B on a scale of 1 day during a 30 day interval when V1 was observing the ISMF. For the fluctuations in all three components of B, SD = 0.010 nT, which gives an upper limit on the fluctuations of the ISMF on the scales observed by V1. This SD rules out the possibility that there is significant power in electromagnetic fluctuations generated by pickup ion ring instabilities at these scales, which strongly constrains models of the IBEX ribbon.