Using Stereoscopic Observations of Cometary Plasma Tails to Infer Solar Wind Speed
Using Stereoscopic Observations of Cometary Plasma Tails to Infer Solar Wind Speed
复制标题
利用彗星等离子体尾部的立体观测来推断太阳风速
DOI：
10.3847/1538-4357/ab93b6
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发表时间：
2020-07
期刊：
影响因子：
--
通讯作者：
Rui Liu
中科院分区：
文献类型：
--
作者：
Long Cheng;Quanhao Zhang;Yuming Wang;Xiaolei Li;Rui Liu
探测太阳附近的太阳风速对于理解太阳风的加热和加速具有重要意义。长期以来，彗星等离子体尾巴一直被用作太阳风速的天然探测器；然而，以前通过等离子体尾巴估计太阳风速的方法是基于单一视角的彗星图像，投影效应可能会影响结果。利用日地关系天文台和太阳/日球层天文台的立体观测资料，我们三维重建了三颗彗星C/2012 S1(ISON)、C/2010 E6和C/2011 W3(LoveJoy)的等离子体尾巴，并推断了周围的太阳风速。第一颗彗星位于高纬度距太阳3.5-6太阳半径(Rs)之间，估计太阳风速约为300-500公里S−1，第二颗彗星位于10 Rs以内，距黄道约20°，估计太阳风速约为200-320公里S−1。第三颗彗星也位于低纬度，但距离太阳较远(-gt；20 Rs)；对于黄道附近的彗星，我们的结果与−模型的预测结果接近，而对于高纬度的彗星，我们的估计结果与模型的结果有显著的偏差。这种一致性和差异性可以用来约束和改进太阳风模型。我们将寻找机会将该方法应用于322P彗星，它的尾巴可能会扫过帕克太阳探测器。
Detection of the solar wind speed near the Sun is significant in understanding the heating and acceleration of the solar wind. Cometary plasma tails have long been used as natural probes for solar wind speed; previous solar wind speed estimates via plasma tails, however, were based on comet images from a single viewpoint, and the projection effect may influence the result. Using stereoscopic observations from the Solar Terrestrial Relations Observatory and the Solar and Heliospheric Observatory, we three-dimensionally reconstruct the plasma tails of three comets C/2012 S1 (ISON), C/2010 E6, and C/2011 W3 (Lovejoy) and infer the ambient solar wind speed. The first comet is located between 3.5 and 6 solar radii (Rs) away from the Sun at high latitudes; the estimated solar wind speed is about 300–500 km s−1. The second comet is located within 10 Rs and about 20° away from the ecliptic; the estimated solar wind speed is about 200–320 km s−1. The third comet is also located at low latitudes but farther (>20 Rs) away from the Sun; the estimated solar wind speed is about 100–600 km s−1. For comets near the ecliptic, our results are close to those predicted by MHD models, whereas for the comet at high latitudes, the deviation between our estimate and the model results is notable. This consistency and difference could be used to constrain and improve solar wind models. We will seek opportunities to apply the method to comet 322P, whose tail may sweep the Parker Solar Probe.
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