共查询到18条相似文献，搜索用时 468 毫秒
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空间飞船Helios 1和Helios 2的磁场探测发现,太阳风高速流中磁场脉动在低频区的能谱的谱指数是随日心距离r而变化的,谱密度的空间梯度是随频率f而变化的,现有关于行星际磁场脉动的理论都不能解释上述现象。本文提出了一个计算行星际磁场能谱径向发展的理论模式。假设在不同频率的脉动之间有由低频向高频传输的能流存在,在这一基础上建立了谱方程,并得到了谱方程的数值解。数值解表明,由0.3AU至1AU,低频区的谱指数增加,而高频区的谱指数近似保持为常数（-1.6）;低频区平均谱密度随着日心距离的变化为r-3.5,在高频区为r-4.1,所有这些都与观测相符合。串级的能量很可能最后传输到质子回旋频率范围,由于回旋共振而耗散,最后加热太阳风质子。这一模式有可能用来计算太阳风的加速问题。 相似文献
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Alfven波在低纬地区电离层的传播有其特殊性,一方面,低纬地区同样存在Alfven速度梯度的巨大变化,导致电离层Alfven谐振器(Ionospheric Alfven resonator, IAR)的形成;另一方面,由于在低纬地区磁倾角很小,所以剪切Alfven波在传播的过程中纬度方向跨度很大,不同纬度电离层参数将共同对其产生影响;并且,由于电离层水平分层,故磁力线与电离层不正交.本文选取双流体力学模型,在忽略场向电场的条件下,利用非正交坐标系,结合IRI07模型与MSISE00模型模拟低纬地区Alfven波的传播,得到其反射及耦合特性.结果表明,低纬地区同样存在电离层Alfven谐振现象,由耦合产生的压缩模有向磁赤道方向传播的趋势,夜间电离层状态相对于白天更适合IAR的形成,谐振频率沿磁力线L值增大单调递增. 相似文献
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采用高精度的拟谱方法，数值模拟了层结海洋中小振幅内行进波的演变和破碎过程.在演变过程中，导致内波破碎的PSI不稳定机制在共振相互作用中逐渐占据主导地位，能量从初级波向低频、高波数运动缓慢传递并形成一次级波包，随即破碎发生.破碎后产生的层化湍流引起的强烈混合以及湍流间歇性可从总能量和涡度峰度随时间的变化趋势看出.我们分析了层化湍流的一些统计特性，包括动能和有效位能沿垂向波数ky的功率谱.结果表明，动能和有效位能谱都存在一个谱段满足k-3y律，且分别可表示为01N4k-3y和02N4k-3y(N为Brunt Visl频率)，通常称其为浮力子区.另外，我们分析了Cox数(湍流扩散系数与分子扩散系数之比)，在层化湍流维持在一定强度时，计算结果和由海洋内区观测(远离内波强生成源和复杂地形)所推测的结论较为吻合. 相似文献
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慢太阳风的起源是一个困扰空间物理领域多年的问题,一些研究人员认为慢太阳风中阿尔芬度比较高的部分起源于小冕洞或者是冕洞的边界,不过另外一些研究者发现高阿尔芬度慢太阳风在成分上和低阿尔芬度的慢太阳风并无显著差别.最近的一项研究中发现的慢太阳风中的小冕洞风并没有特别高的阿尔芬度.我们利用一个简单的二维太阳风模型计算了阿尔芬波和小冕洞风的传播;计算结果显示,由于阿尔芬波的传播特性,从小冕洞出发的等离子体和阿尔芬波动在传播到1AU的过程中会发生分离,形成了低阿尔芬度的小冕洞风和高阿尔芬度的普通慢风.这个结果定性地解释了慢太阳风中观测到的小冕洞风和高阿尔芬度慢风的特性,也为解开慢太阳风的起源之谜提供了新的思路. 相似文献
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对流边界层顶部特性的对流槽实验模拟研究 总被引：5，自引：1，他引：5
利用对流槽研究对流边界层的顶部特性.实验结果表明,产生于混合层的上冲热泡可在对流边界层顶上的覆盖逆温层中激发出重力波;夹卷层的湍流结构表现出各向异性,水平尺度大于垂直尺度,与混合层中的湍流结构明显不同;利用可视图像直观显示了夹卷过程,夹卷层的温度谱表现出独特的结构特征,湍流能谱有明显的分区现象,谱幂率与现有理论分析结果有较大偏离.在实验结果的基础上,提出了关于夹卷速率的新参数化方案,夹卷速率可由地面热通量、混合层高度和覆盖逆温强度确定,方案中的系数C由实验测量数据拟合得出:C=0.95,与Deardroff等的对流槽实验数据的拟合结果(C=1.11)非常接近. 相似文献
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Resonant transformation of fast magnetosonic (FMS) wave flux into Alfven and slow magnetosonic (SMS) oscillations is investigated in the one-dimensionally inhomogeneous magnetosphere. Spatial distribution of energy absorption rate of FMS oscillations penetrating into the magnetosphere from the solar wind is studied. The FMS wave energy absorption rate caused by magnetosonic resonance excitation is shown to be several orders of magnitude greater than that caused by Alfven resonance excitation at the same surface. It is connected with the spectrum of incident FMS waves. The Kolmogorov spectrum is used in numerical calculations. Magnitude of the Fourier harmonics exciting resonant Alfven oscillations is much smaller than that of the harmonics driving lower-frequency magnetosonic resonance. It is shown that resonant transformation of FMS waves into SMS oscillations can be an effective mechanism of energy transfer from the solar wind to the magnetosphere. 相似文献
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本文将太阳风涨落传输能量产生磁层亚暴的机制推广到无碰撞等离子体过程。太阳风的涨落在磁层顶激发压缩阿尔文波,并在磁尾的无碰撞等离子体中传播。尾瓣中满足条件β?1,而等离子体片中β≥1,其中β为等离子体压力与磁压之比。这样,快磁声波在尾瓣中几乎不衰减,而在等离子体片中很快衰减,将波动能量耗散在等离子体片中使等离子体加热或者粒子加速。这种机制还表明,磁尾等离子体片中的高能粒子可以由太阳风涨落动能耗散而被加速,不一定是直接源于太阳。 相似文献
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L. S. Rakhmanova M. O. Riazantseva N. L. Borodkova O. V. Sapunova G. N. Zastenker 《Geomagnetism and Aeronomy》2017,57(6):664-671
Data from the BMSW spectrometer, which measures the ion flux value and sometimes plasma parameters with a time resolution of 31 ms, allow the study of the parameters of turbulence of the solar wind and magnetosheath plasma on kinetic scales. In this work, the frequency spectra of the ion flux fluctuations before and after recording the interplanetary shock front in the Earth’s magnetosheath are compared based on these data. It is shown that, in contrast to the solar wind, where the exponential decay of the spectrum often occurs after the shock front on the kinetic scales, no such phenomenon is observed in the magnetosheath: the spectrum on these scales can be approximated by a power function in all the cases considered. In half of these cases, the spectrum slope on the kinetic scales does not change during the interplanetary shock propagation. The results indicate a weak impact of interplanetary shock waves on the parameters of the plasma turbulence. In addition, it is shown that an interplanetary shock does not change the level of intermittency of the ion flux in the magnetosheath at both low and high level before the front. 相似文献
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N. M. Gavrilov 《Annales Geophysicae》1997,15(12):1570-1580
The mechanism of generation of internal gravity waves (IGW) by mesoscale turbulence in the troposphere is considered. The equations that describe the generation of waves by hydrodynamic sources of momentum, heat and mass are derived. Calculations of amplitudes, wave energy fluxes, turbulent viscosities, and accelerations of the mean flow caused by IGWs generated in the troposphere are made. A comparison of different mechanisms of turbulence production in the atmosphere by IGWs shows that the nonlinear destruction of a primary IGW into a spectrum of secondary waves may provide additional dissipation of nonsatu-rated stable waves. The mean wind increases both the effectiveness of generation and dissipation of IGWs propagating in the direction of the wind. Competition of both effects may lead to the dominance of IGWs propagating upstream at long distances from tropospheric wave sources, and to the formation of eastward wave accelerations in summer and westward accelerations in winter near the mesopause. 相似文献
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《Journal of Atmospheric and Solar》2000,62(4):239-248
Based on long-term observations of the resonance structure in the electromagnetic background noise spectrum (resonance spectrum structure, RSS), recorded in the frequency range 0.1–10 Hz over one complete solar cycle (11 years, from 1985 to 1995), it was found that the resonance conditions for Alfven waves in the ionosphere (ionospheric Alfven resonator) are determined at midlatitudes by the level of solar activity. RSS are regularly observed in years of minimum solar activity, and are practically absent in years of maximum solar activity. It is shown that consideration of the ionospheric Alfven resonator explains the dependence of the RSS on solar activity. 相似文献
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Ulysses 是迄今为止第一次沿独特的日球纬度方向考察日球高纬度空间区域的飞船。本文描述了 Ulysses 飞船的部分主要观测结果,并进行了分析,在 Ulysses 飞船穿越太阳南,北极之前,科学家们提出了各种不同的太阳风速度、磁场等参量的纬向变化模型。分析表明,这些模型都不能解释 Ulysses 飞船的观测结果。Ulysses 飞船的观测对经典的太阳风理论提出了挑战,太阳风的加热与加速是一个远没有被解决的问题。观测与分析表明,经典热传导不可能驱动高速流,太阳风的加速伴随着加热的发生,而加热率大小可能与离子的回旋频率有关;太阳风的热源可能不是单一的形式,而且不同形式的热源对太阳的加热贡献大小与日球径向距离有关。本文讨论并分析了几种可能的太阳风加热与加速机制。 相似文献
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This paper considers the features of turbulent characteristics of ion flux variations in the solar wind and magnetosheath at the scale of 0.01–10 Hz based on measurements on the BMSW plasma spectrometer (Plasma-F experiment) mounted on the Spektr-R satellite. A variability of types of fluctuation frequency spectra is shown. Fluctuation spectra with certain features in the transition region from the inertial to the dissipative range are selected (a sharp knee in the fluctuation spectrum, plateau and peak in the knee, and a nonlinear spectrum bend at high frequencies). The degree of difference between the observed spectra and the spectra characteristic of the developed isotropic turbulence in the Kolmogorov model is determined. The probability of observation of the spectra of certain types is estimated. The features of fluctuation spectra in the solar wind and magnetosheath are compared for each type of spectra. 相似文献