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Surface waves on Saturn's magnetopause

机译：土星的磁层顶上的表面波

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摘要

Waves on the surface of a planetary magnetopause promote energy transport into the magnetosphere, representing an important aspect of solar wind-magnetosphere coupling. At Saturn's magnetopause it has been proposed that growth of the Kelvin-Helmholtz (K-H) instability produces greater wave activity on the dawn side of the surface than on the dusk side. We test this hypothesis using data taken by the Cassini spacecraft during crossings of Saturn's magnetopause. Surface orientation perturbations are primarily controlled by the local magnetospheric magnetic field orientation, and are generally greater at dusk than at dawn. 53% of all crossings were part of a sequence of regular oscillations arising in consecutive surface normals that is strong evidence for tailward propagating surface waves, with no detectable local time asymmetry in this phenomenon. We estimate the dominant wave period to be ～ 5 h at dawn and ～3 h at dusk. The role played by the magnetospheric magnetic field, tailward wave propagation, and the dawn-dusk difference in wave period suggests that K-H instability is a major wave driving mechanism. Using linear K-H theory we estimate the dominant wavelength to be ～10 Saturn radii (R_s) and amplitude to be ～1 R_s at both dawn and dusk, giving propagation speeds of ～30 and ～50 km s~(-1) at dawn and dusk, respectively. The lack of the hypothesized dawn-dusk asymmetry in wave activity demonstrates that we need to revise our understanding of the growth of the K-H instability at Saturn's magnetopause, which will have implications for the study of other planetary magnetospheres.
机译：行星磁层顶表面上的波促进能量传输到磁层，这代表了太阳风-磁层耦合的一个重要方面。在土星的磁层顶，有人提出，开尔文-亥姆霍兹（K-H）不稳定性的增长在表面的曙光一侧比黄昏的一侧产生更大的波浪活动。我们使用卡西尼号飞船在土星的磁层顶穿越过程中获得的数据来检验这个假设。表面取向的扰动主要由局部磁层磁场取向控制，通常在黄昏时比在黎明时大。所有交叉中的53％是连续表面法线中出现的规则振动序列的一部分，这是向后传播的表面波的有力证据，在这种现象中没有可检测到的局部时间不对称。我们估计主波周期为黎明时〜5 h，黄昏时〜3 h。磁层磁场，尾波传播和波周期中的黎明-黄昏差异所起的作用表明，K-H不稳定性是主要的波驱动机制。使用线性KH理论，我们估计在黎明和黄昏时主波长为〜10土星半径（R_s），振幅为〜1 R_s，在黎明和黄昏时的传播速度分别为〜30和〜50 km s〜（-1）。分别黄昏。缺乏假设的波活动中的黎明-黄昏不对称性表明，我们需要修改对土星磁层顶K-H不稳定性增长的理解，这将对其他行星磁层的研究产生影响。

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  • 来源
    《Planetary and space science》 |2012年第1期|p.109-121|共13页
  • 作者

    A. Masters; N. Achilleos; J.C. Cutler; A.J. Coates; M.K. Dougherty; G.H. Jones;

  • 作者单位

    Milliard Space Science Laboratory, Department of Space and Climate Physics, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK,The Centre for Planetary Sciences at UCL/Birkbeck, Cower St., London, WC1E 6BT, UK;

    The Centre for Planetary Sciences at UCL/Birkbeck, Cower St., London, WC1E 6BT, UK,Atmospheric Physics Laboratory, Department of Physics and Astronomy, University College London, Cower Street, WC1E 6BT, UK;

    Space and Atmospheric Physics Croup, The Blackett Laboratory, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK;

    Milliard Space Science Laboratory, Department of Space and Climate Physics, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK,The Centre for Planetary Sciences at UCL/Birkbeck, Cower St., London, WC1E 6BT, UK;

    Space and Atmospheric Physics Croup, The Blackett Laboratory, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK;

    Milliard Space Science Laboratory, Department of Space and Climate Physics, University College London, Holmbury St. Mary, Dorking, Surrey, RH5 6NT, UK,The Centre for Planetary Sciences at UCL/Birkbeck, Cower St., London, WC1E 6BT, UK;

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  • 正文语种 eng
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  • 关键词

    saturn; magnetopause; surface waves; solar wind-magnetosphere interaction; kelvin-helmholtz instability;

    机译：土星磁停表面波太阳风-磁层相互作用开尔文-亥姆霍兹不稳定性;

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