论文标题
估算振荡冠状环的湍流估计{kelvin-helmholtz的不稳定性}的能量耗散}
Estimating the energy dissipation {from Kelvin-Helmholtz instability induced} turbulence in oscillating coronal loops}
论文作者
论文摘要
开尔文 - 赫尔姆霍尔兹{不稳定性}湍流是一种有前途的机制，可以通过MHD波加热太阳能电晕中的回路。在本文中，我们介绍了{kelvin-helmholtz不稳定}湍流$ \ varepsilon _ {\ rm d} $的耗散速率的分析模型，发现它是波振幅（$ d $）的缩放（$ \ varepsilon _ {$ \ varepsilon _ {$ \ varepsilon _ {\ rm rm rm d prop d prop prop d prop）。基于稳态湍流的概念，我们期望在{}回路的整个体积中加热湍流加热与通过其脚步注入的总能量相匹配。在这种情况下，波幅度必须随着注入能量的立方根而变化。将分析结果与模拟的结果进行比较，表明我们的分析配方从数值工作中捕获了湍流耗散的关键方面。将该模型应用于观察到的衰减扭结波的特征，我们预测这些观察到的波的幅度不足以湍流加热太阳能电晕。
Kelvin-Helmholtz {instability induced} turbulence is one promising mechanism by which loops in the solar corona can be heated by MHD waves. In this paper we present an analytical model of the dissipation rate of {Kelvin-Helmholtz instability induced} turbulence $\varepsilon_{\rm D}$, finding it scales as the wave amplitude ($d$) to the third power ($\varepsilon_{\rm D}\propto d^3$). Based on the concept of steady-state turbulence, we expect the turbulence heating throughout the volume of {the} loop to match the total energy injected through its footpoints. In situations where this holds, the wave amplitude has to vary as the cube-root of the injected energy. Comparing the analytic results with those of simulations shows that our analytic formulation captures the key aspects of the turbulent dissipation from the numerical work. Applying this model to the observed characteristics of decayless kink waves we predict that the amplitudes of these observed waves is insufficient to turbulently heat the solar corona.
