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首页> 外文期刊>Planetary and space science >Titan's highly dynamic magnetic environment: A systematic survey of Cassini magnetometer observations from flybys TA-T62
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Titan's highly dynamic magnetic environment: A systematic survey of Cassini magnetometer observations from flybys TA-T62

机译：土卫六的高动态磁环境：飞越TA-T62对卡西尼磁力计观测结果的系统调查

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摘要

We analyze the variability of the ambient magnetic field near Titan during Cassini encounters TA-T62 (October 2004-October 2009). Cassini magnetometer (MAG) data show that the moon's magnetic environment is strongly affected by its proximity to Saturn's warped and highly dynamic magnetodisk. In the nightside sector of Saturn's magnetosphere, the magnetic field near Titan is controlled by intense vertical flapping motions of the magnetodisk current sheet, alternately exposing the moon to radially stretched lobe-type fields and to more dipolar, but highly distorted current sheet fields. In southern summer, when most of the Cassini encounters took place, the magnetodisk current sheet was on average located above Titan's orbital plane. However, around equinox in August 2009, the distortions of Titan's magnetic environment due to the rapidly moving current sheet reached a maximum, thus suggesting that the equilibrium position of the sheet at that time was significantly closer to the moon's orbital plane. In the dayside magnetosphere, the formation of the magnetodisk lobes is partially suppressed due to the proximity of the magnetopause. Therefore, during most encounters that took place near noon, Titan was embedded in highly distorted current sheet fields. Within the framework of this study, we not only provide a systematic classification of all Titan flybys between October 2004 and October 2009 as lobe-type or current sheet scenarios, but we also calculate the magnetospheric background field near Titan's orbit whenever possible. Our results show that so far, there is not a single Cassini flyby that matches the frequently applied picture of Titan's plasma interaction from the pre-Cassini era (background field homogeneous, stationary and perpendicular to the moon's orbital plane). The time scales upon which the ambient magnetospheric field close to Titan undergoes significant changes range between only a few minutes and up to several hours. The implications for the development of numerical models for Titan's local plasma interaction are discussed as well.
机译：我们分析了卡西尼号遇到TA-T62（2004年10月至2009年10月）期间土卫六附近环境磁场的变化。卡西尼号磁强计（MAG）的数据表明，月球的磁环境受到其与土星弯曲且高度动态的磁磁盘的接近程度的强烈影响。在土星磁层的夜间区域，土卫六附近的磁场是由磁碟电流板的强烈垂直拍动控制的，交替地使月球暴露于径向拉伸的波瓣型场和更偶极但高度失真的电流板场。在南部的夏季，当大多数卡西尼号遭遇时，磁碟电流片平均位于土卫六的轨道平面上方。然而，在2009年8月春分前后，由于快速移动的电流片而导致的泰坦磁场环境的畸变达到最大，因此表明当时该片的平衡位置明显更靠近月球的轨道平面。在白天的磁层中，由于磁层顶的接近，部分地抑制了磁盘凸角的形成。因此，在中午附近发生的大多数encounter碰中，Titan都嵌入了高度扭曲的当前工作表字段中。在这项研究的框架内，我们不仅将2004年10月至2009年10月之间所有土卫六飞越作为叶状或当前表层情景进行了系统分类，而且还尽可能计算了土卫六轨道附近的磁层背景场。我们的结果表明，到目前为止，还没有一个卡西尼飞越能与卡西尼前时代（背景场均匀，静止且垂直于月球轨道平面）泰坦的等离子相互作用的常用图像相匹配。接近土卫六的环境磁层磁场发生重大变化的时间范围仅在几分钟到几小时之间。还讨论了开发土卫六局部等离子体相互作用的数值模型的意义。

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