帕克太阳探测器与太阳轨道器对太阳风统计能量收支的研究：1 - 不平衡总能量的径向演化
Statistical Energy Budget of the Solar Wind with Parker Solar Probe and Solar Orbiter : 1 - Unbalanced Total Energy Radial Evolution
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中文总结 AI 辅助
该研究利用帕克太阳探测器与太阳轨道器的观测数据，检验大尺度非线性理想MHD能量收支的有效性，发现14至203太阳半径间总能量增56%，暗示理论或忽略太阳风加速的重要能量项。
中文摘要 AI 辅助
长期以来，磁流体动力学（MHD）描述一直被视为研究太阳风加热与加速问题最成功的框架之一。在一系列简化假设下，该理论提供了简化的大尺度描述，被广泛用于研究电磁波动在太阳风能量收支中的能量作用。但实际上，与精确方程组相比，对MHD进行简化会导致部分物理信息的丢失。而观测得到的能量收支可帮助我们验证简化过程中是否丢失了能量相关信息。为此，我们利用帕克太阳探测器（PSP）与太阳轨道器（SO）的太阳风观测数据，直接检验大尺度非线性理想MHD能量收支的有效性。在通过与以往相似太阳风特性研究的对比验证测量可靠性后，我们检验了MHD理论预测的总能量守恒性。我们发现，在14至203个太阳半径范围内，平均总能量随径向距离增加了56%（±9%）；动能的增加无法被热能与电磁贡献的减少充分补偿。我们调查了观测不确定性的主要来源，发现这些不确定性无法解释观测到的能量增加。这些结果表明，大尺度理论描述可能忽略了对太阳风加速具有重要能量贡献的项。假设该贡献存在，我们预测这一额外能量将随径向距离按r^(-0.54±0.38)的比例变化。
英文摘要
The magneto-hydrodynamic (MHD) description of the solar wind has long been regarded as one of the most successful frameworks for investigating solar wind heating and acceleration. Under a set of simplifying assumptions, it provides a reduced large-scale description that is widely used to study the energetic role of electromagnetic fluctuations in the solar wind energy budget. In practice, applying simplification to MHD can result in the loss of some physics compared to an exact set of equations. However, an observational energy budget can help us to verify whether any energetic information has been lost in the process of simplification. To do so, we directly test the validity of the large-scale non-linear ideal MHD energy budget with solar wind observations from Parker Solar Probe (PSP) and Solar Orbiter (SO). After verifying the reliability of the measurements through comparison with previous studies of similar solar wind properties, we test the conservation of the total energy predicted by the MHD theory. We find that the average total energy increases with radial distance by $56\%$ ($\pm9\%$) between 14 and 203 solar radii. The increase in kinetic energy is not sufficiently compensated by the decrease of the thermal and electromagnetic contributions. We investigate the major sources of observational uncertainty and find that they cannot account for the observed energy increase. These results suggest that the large-scale theoretical description may neglect an energetically significant contribution to solar wind acceleration. Assuming that such a contribution exists, we predict that this extra energy would scale with radial distance as $r^{-0.54\pm0.38}$.
发表机构
- University of California, Berkeley（加州大学伯克利分校）
- Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris（巴黎天文台，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎大学）
- IRAP, Observatoire Midi-Pyrénées, Université Toulouse III - Paul Sabatier, CNRS（红外与射电天文研究所，南比利牛斯天文台，图卢兹第三大学-保罗·萨巴蒂尔大学，法国国家科学研究中心）
- Imperial College London（帝国理工学院）
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