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首页> 外文期刊>Journal of Geophysical Research. Biogeosciences >Cyclotron resonance in coronal holes 3. A five-beam turbulence-driven model
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Cyclotron resonance in coronal holes 3. A five-beam turbulence-driven model

机译：回旋加速器在冠状孔中的共振3.五束湍流驱动模型

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Following Hollweg and Johnson [1988], Isenberg [1990], and Li et al. [1999a], we postulate that the Sun launches a flux of low-frequency Alfven waves, which dissipate via a turbulent cascade to high frequencies where the energy is absorbed by ion cyclotron resonant interactions. The plasma consists of two proton beams, which are proxies for the resonant and nonresonant halves of their distribution function, two He++ beams, which are proxies for the strongly and weakly resonant halves of their distribution, and a single beam of O+5 with vanishing density. The level of the power spectrum at the high resonant frequencies is determined by the condition that the protons and He++ resonantly absorb energy at the same rate at which the low-frequency waves are dissipating. Once the level of the high-frequency power spectrum is determined, the resonant heating and acceleration of the O+5 can be calculated. For both Kolmogorov and Kraichnan scalings of the turbulent dissipation the model yields results for the protons that are in reasonably good agreement with the UVCS/SOHO results. The He++ becomes; more than mass proportionally heated and flows faster than the protons, close to the Sun. However, our model is unable to reproduce the UVCS/SOHO observation that the O+5 temperature is still increasing with heliocentric distance r out to 3.5 r(s). Instead, the O+5 becomes very hot initially, experiences a strong mirror force, and accelerates to high speed, which in turn leads to rapid adiabatic cooling. Put another way, the O+5 observations imply that (dT(perpendicular to)/dt)(res) must bean increasing function of r, while it is the nature of the resonant interactions to make (dT(perpendicular to)/dt)(res) decrease with increasing r. [References: 66]
机译：继Hollweg和Johnson [1988]，Isenberg [1990]和Li等人。 [1999a]，我们假设太阳发射了低频Alfven波，它通过湍流级联消散到高频，在高频中能量被离子回旋加速器的共振相互作用吸收。等离子体由两个质子束和两个He ++束组成，这两个质子束分别代表它们的分布函数的共振和非共振半部分，两个He ++束分别代表其分布函数的强和弱共振的一半，而O + 5的单个束则消失密度。质子和He ++共振吸收能量的频率与消散低频波的速率相同，因此可以确定高共振频率处的功率谱水平。一旦确定了高频功率谱的水平，就可以计算出O + 5的共振发热和加速度。对于湍流耗散的Kolmogorov和Kraichnan标度，该模型得出的质子结果与UVCS / SOHO结果相当吻合。 He ++变成了;接近太阳的质量比按比例加热的质量大，并且比质子的流动快。但是，我们的模型无法重现UVCS / SOHO的观察结果，即O + 5温度仍随着日心距r至3.5 r（s）的增加而增加。取而代之的是，O + 5最初会变得很热，经受强大的镜面力，然后加速至高速，从而导致快速的绝热冷却。换句话说，O + 5观测表明（dT（垂直于/ dt）（res）必须具有r的递增函数，而这是共振相互作用的本质（dT（垂直于/ dt）/ dt） （res）随着r的增加而减少。 [参考：66]

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