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Influence of a uniform coronal magnetic field on solar p modes: coupling to slow resonant MHD waves

机译：日冕均匀磁场对太阳p模式的影响：耦合至慢速共振MHD波

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摘要

The influence of a constant coronal magnetic field on solar global oscillations is investigated for a simple planar equilibrium model. The model consists of an atmosphere with a constant horizontal magnetic field and a constant sound speed, on top of an adiabatic interior having a linear temperature profile. The focus is on the possible resonant coupling of global solar oscillation modes to local slow continuum modes of the atmosphere and the consequent damping of the global oscillations. In order to avoid Alfvén resonances, the analysis is restricted to propagation parallel to the coronal magnetic field. Parallel propagating oscillation modes in this equilibrium model have already been studied by Evans and Roberts (1990). However, they avoided the resonant coupling to slow continuum modes by a special choice of the temperature profile. The physical process of resonant absorption of the acoustic modes with frequency in the cusp continuum is mathematically completely described by the ideal MHD differential equations which for this particular equilibrium model reduce to the hypergeometric differential equation. The resonant layer is correctly dealt with in ideal MHD by a proper treatment of the logarithmical branch cut of the hypergeometric function. The result of the resonant coupling with cusp waves is twofold. The eigenfrequencies become complex and the real part of the frequency is shifted. The shift of the real part of the frequency is not negligible and within the limit of observational accuracy. This indicates that resonant interactions should definitely be taken into account when calculating the frequencies of the global solar oscillations.
机译：对于简单的平面平衡模型，研究了恒定日冕磁场对太阳整体振荡的影响。该模型由具有恒定水平磁场和恒定声速的气氛组成，并在具有线性温度曲线的绝热内部之上。重点是整体太阳振荡模式可能与大气的局部慢连续谱模式发生共振耦合，以及由此产生的整体振荡阻尼。为了避免Alfvén共振，分析仅限于平行于日冕磁场的传播。埃文斯和罗伯茨（1990）已经研究了这种平衡模型中的并行传播振荡模式。但是，他们通过特殊选择温度曲线避免了共振耦合到慢速连续模式。用理想的MHD微分方程在数学上完整地描述了尖峰连续谱中具有频率的声模的共振吸收的物理过程，对于理想的MHD微分方程，该方程简化为超几何微分方程。通过适当处理超几何函数的对数分支切线，可以在理想的MHD中正确处理谐振层。尖峰波谐振耦合的结果是双重的。本征频率变得复杂，并且频率的实部发生了变化。频率实部的偏移不可忽略，并且在观测精度的范围内。这表明在计算整体太阳振荡的频率时，一定要考虑共振相互作用。

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  • 来源
    《Solar Physics》 |2002年第1期|1-24|共24页
  • 作者

    P. Vanlommel; A. Debosscher; J. Andries; M. Goossens;

  • 作者单位

    Centre for Plasma Astrophysics K.U;

    Centre for Plasma Astrophysics K.U;

    Centre for Plasma Astrophysics K.U;

    Centre for Plasma Astrophysics K.U;

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  • 正文语种 eng
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