泰坦的原子和分子氮环
Titan's Atomic and Molecular Nitrogen Tori
摘要：
Shematovich等人（2003年）最近表明，泰坦大气中的等离子体诱导溅射是土星磁层中中性氮的来源，与光解离源相当。这些来源形成了一个环形的氮云，大致以泰坦的轨道半径为中心，但受到土星的引力束缚。一旦电离，这些粒子有助于土星的等离子体。当土卫六位于土星的磁层顶时，新形成的离子可以向内扩散，成为磁层内的高能氮，在那里它们可以溅射并注入冰冷的卫星表面。我们的三维模拟产生了第一个一致的泰坦产生的N和N2中性云;太阳紫外线辐射和磁层等离子体使这些粒子解离和电离。云的形态和相关的氮等离子体源率预测卡西尼数据的预期。由于土卫六通过光分解喷射出的分子氮的量很小，卡西尼号探测到的分子氮离子将是大气溅射的一个指标。
英文摘要：
Shematovich et al. (2003) recently showed plasma induced sputtering in Titan's atmosphere is a source of neutral nitrogen in Saturn's magnetosphere comparable to the photo-dissociation source. These sources form a toroidal nitrogen cloud roughly centered at Titan's orbital radius but gravitationally bound to Saturn. Once ionized, these particles contribute to Saturn's plasma. When Titan is inside Saturn's magnetopause, newly formed ions can diffuse inward becoming inner magnetospheric energetic nitrogen where they can sputter and be implanted into icy satellite surfaces. Our 3-D simulation produces the first consistent Titan generated N and N2 neutral clouds; solar UV radiation and magnetospheric plasma subject these particles to dissociation and ionization. The cloud morphologies and associated nitrogen plasma source rates are predicted in anticipation of Cassini data. Since the amount of molecular nitrogen ejected from Titan by photo-dissociation is small, molecular nitrogen ions detection by Cassini will be an indicator of atmospheric sputtering.
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