Energetic particle measurements in the vicinity of Dione during the three Cassini encounters 2005–2011
Energetic particle measurements in the vicinity of Dione during the three Cassini encounters 2005–2011
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2005-2011 年卡西尼号三次遭遇期间土卫四附近的高能粒子测量
DOI：
10.1016/j.icarus.2013.06.007
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发表时间：
2013
期刊：
影响因子：
3.2
通讯作者：
K. Khurana
中科院分区：
文献类型：
--
作者：
N. Krupp;E. Roussos;H. Kriegel;P. Kollmann;M. Kivelson;A. Kotova;C. Paranicas;D. Mitchell;S. Krimigis;K. Khurana
卡西尼号太空船在2005年至2011年期间三次遇到土卫四。在飞越期间，进行了粒子和场测量，并用于研究土星系统中第四大卫星与周围磁层等离子体之间的磁层相互作用。在这里，我们提出的结果的低能磁层测量系统（LEMMS），磁层成像仪器MIMI的一部分，测量高能离子和电子超过20千电子伏到几兆电子伏和结果的磁力计仪器（MAG）板载的航天器。在土卫四附近被捕获的粒子在土星的磁层中反弹和漂移，最终消失在月球表面。吸收特征的位置和深度取决于物种、它们的能量和飞越的几何形状。只有对上游飞越D1的能量依赖的离子吸收签名测量，我们得出结论，质子存在于上游区域可以解释所观察到的辍学功能。另外两个探测器D2和D3穿过了月球的几何尾迹。在每一次遭遇中，我们都观察到了电子通量中的吸收特征，这些电子通量是由这些粒子在土星磁层中漂移运动时损失到月球上造成的。这些吸收特征的轮廓是依赖于能量的，并且在能量高于约100 keV时，在月球尾流的planeplane和anti-planeplane扇区之间变得不对称。我们比较这些电子尾流剖面与电子导引中心轨迹跟踪在模拟环境中的狄俄涅的磁层相互作用使用的“自适应混合模型空间等离子体模拟（A.I.K.E.F.）”。我们的结果表明，在Dione的相互作用区域的磁场和电场扰动，以及磁层扩散需要考虑，以解释在不同能量的高能电子数据的功能。
The Cassini spacecraft encountered the moon Dione three times between 2005 and 2011. During the flybys particles and fields measurements have been performed and used to study the magnetospheric interaction between the fourth largest moon in the saturnian system and the surrounding magnetospheric plasma. Here we present the results of the Low Energy Magnetospheric Measurement System (LEMMS), part of the Magnetospheric Imaging Instrument MIMI, measuring energetic ions and electrons above 20 keV up to several MeV and results from the magnetometer instrument (MAG) onboard the spacecraft. The trapped particles in the vicinity of Dione bounce and drift in Saturn’s magnetosphere and eventually are lost onto the surface of the moon. The location and depth of the absorption signature depends on species, their energy and on the geometry of the flyby. Only for the upstream flybyD1were energy-dependent ion absorption signatures measured and we conclude that protons present in the upstream region can explain the observed dropout features. The other two encountersD2andD3went through the moon’s geometrical wake. During each of the encounters we observed absorption signatures in the fluxes of electrons caused by losses of those particles onto the moon during their drift motion in the saturnian magnetosphere. The profile of these absorption signatures is energy dependent, and becomes asymmetric between the planetward and anti-planetward sectors of the moon’s wake at energies above about 100 keV. We compare these electron wake profiles with ones resulting from electron guiding center trajectory tracings in a simulated environment of Dione’s magnetospheric interaction using the “Adaptive hybrid model for space plasma simulations (A.I.K.E.F.)”. Our results indicate that the magnetic and electric field perturbations in Dione’s interaction region, as well as magnetospheric diffusion need to be taken into account in order to explain the features of the energetic electron data at different energies.
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