Solar faculae and waves propagating in the solar atmosphere

Solar faculae are among the most common manifestations of solar activity and can play an important role in the energy transfer from the lower solar atmosphere into the corona. However, the mechanisms by which energy is transferred remain insufficiently studied. Our work is based on observational data obtained with the AST telescope of the Sayan solar observatory. Simultaneous observations were performed in the Hα 6563 Å and FeI 6569 Å, BaII 4554 Å and FeI 4551.6 Å, and CaII 8542 Å and FeI 8538 Å pairs of spectral lines. The studies indicated that the spectral composition of the line-of-sight (LOS) velocity oscillations in faculae is inhomogeneous and is affected by the chromospheric network’s structural elements. The possible presence of short and low magnetic loops in the facula region makes it difficult to determine the unambiguous phase relations between chromospheric and photospheric oscillations. The LOS velocity oscillation signals registered at the chromospheric level both lead and lag behind the signals registered at the photospheric level. At the same time, signs of propagating waves are evidently registered in the chromosphere of individual faculae.     

Wind control of the propagation of acoustic gravity waves in the polar atmosphere

The relationship between the directions of polar acoustic gravity waves and a wind at 250–350 km altitudes has been studied based on an analysis of the Dynamics Explorer 2 satellite measurements. A method, which makes it possible to determine the direction of these waves relative to the satellite velocity vector based on one-point measurements of different neutral atmosphere parameters, is presented. It has been established that acoustic gravity waves observed over the polar caps systematically propagate upwind, which argues for their spatial wind filtering. In the polar regions, waves mainly propagate in two directions: toward magnetic noon and 15–16 MLT. Waves tend to move counterclockwise and clockwise over the northern and southern polar caps, respectively.     

Peculiarities of energy transport in the atmosphere by acoustic gravity waves

The dependence of energy transport by acoustic gravity waves (AGWs) on their spectral properties is studied. On the basis of the analysis of expressions for group velocities and energy fluxes of AGWs, it is shown that there exist separate frequencies and wavelengths at which the energy transport in space is most efficient. Comparison of the obtained results with the data of observations on board the Dynamic Explorer 2 satellite shows that, in the upper atmosphere of the Earth’s polar regions, AGWs with spectral parameters corresponding to the maximum of energy transport predominate.     

General-planetary character of three-dimensional planetary waves propagation in lower and upper Earth atmosphere

A new branch of planetary Rossby waves is found taking into account latitudinal gradient of horizontal component of the earth rotation's angular velocity. Frequencies of a new branch and ordinary Rossby waves numerically coincide but strongly differ on character of dispersion. The general condition naturally “filtering” planetary waves in the long-wave approximation and internal inertial waves in the short-wave approximation was established.     

Using the nonlinear geometrical acoustics method in the problem of moreton and EUV wave propagation in the solar corona

Propagation of shock related Moreton and EUV waves in the solar atmosphere is simulated by the nonlinear geometrical acoustics method. This method is based on the ray approximation and takes account of nonlinear wave features: dependence of the wave velocity on its amplitude, nonlinear dissipation of wave energy in the shock front, and the increase in its duration with time. The paper describes ways of applying this method to solve the propagation problem of a blast magnetohydrodynamic shock wave. Results of analytical modeling of EUV and Moreton waves in the spherically symmetric and isothermal solar corona are also presented. The calculations demonstrate deceleration of these waves and an increase in their duration. The calculation results of the kinematics of the EUV wave observed on the Sun on January 17, 2010 are presented as an example.     

Ejection and descent of matter in the solar atmosphere

The descent and ejection of matter in the solar atmosphere observed in the CaII 8498-Å line have been studied. In the NOAA active region no. 10 792 on July 30, 2005 before the flare, the dense cold gas cloud descended with a ray velocity of ～8 km/s and then ascended in the impulsive phase. The plasma ascended with an acceleration reaching 0.4 km/s² in the flare maximum. The acceleration of the matter likely continued after the flare maximum, because an acceleration of higher than 0.5 km/s² was required for the appearance of the ejection at the edge of the occulting disk of the LASCO C2 coronagraph at 0557 UT. The descent of the matter resulting in the local heating of the chromosphere was also observed in the NOAA active region no. 10656 on August 9, 2004 before the flare. The maximum descent velocity was no more than 24.7 km/s.     

Planetary waves in coupling the lower and upper atmosphere

The purpose of the paper is to answer the question if planetary waves (PW) are capable of propagating into the thermosphere. First the simplest vertical structure equation of the classic tidal theory accounting for a realistic vertical temperature profile is considered. Analysis and simulation show that the well-known normal atmospheric modes (NM), which are trapped in the lower and middle atmosphere, exhibit a wave-like vertical structure with a large vertical wavelength in the thermosphere. Moreover, the reflection of these modes from the vertical temperature gradient in the lower thermosphere causes appearance of the wave-energy upward flux in the middle atmosphere, and in a linearized formulation this flux is constant above the source region. To investigate a possibility of the NM forcing by stratospheric vacillations and to consider the propagation of different PW up to the heights of the upper thermosphere, a set of runs with a mechanistic Middle and Upper Atmosphere Model has been performed. The results of the simulation show that quasi-stationary and longer-period PW are not able to penetrate into the thermosphere. The shorter-period NM and ultra-fast Kelvin wave propagate up to the heights of the lower thermosphere. However, above about 150 km they are strongly suppressed by dissipative processes. The role of the secondary waves (nonmigrating tides) arising from nonlinear interaction between the primary migrating tides and quasi-stationary PW is discussed. We conclude that PW are not capable of propagating directly up to the heights of the ionospheric F2 region. It is suggested that other physical processes (for instance, the electrostatic field perturbations) have to be taken into account to explain the observed PW-like structures in ionospheric parameters.     

基于黏弹滑移界面理论揭示套管中模式波的传播特征

目前固井质量评价主要是利用套管中模式波的幅度或衰减变化判断套管与水泥间的胶结状况.在超声测量频段（70~500 kHz）,现有声波测井仪器工作时在套管中激发的模式波类似薄板中的对称兰姆波（拉伸波）或反对称兰姆波（弯曲型兰姆波）.本文将黏弹滑移界面理论应用到套管和水泥的耦合界面,探讨了套管中的准兰姆波（包括拉伸波和弯曲型兰姆波）与套管后物质的耦合方式,拉伸波与套后物质主要以剪切刚度耦合,即便是0.01 mm的微环也会使得拉伸波的衰减明显降低,接近套后是流体时的响应特征;而弯曲型兰姆波与套管后物质主要以法向刚度耦合,这使得在套后胶结轻质水泥时弯曲型兰姆波对微环不敏感,在套后耦合常规水泥时微环的存在又会使得弯曲型兰姆波的衰减明显增强,衰减的增加说明其与套后物质的声耦合更紧密,也表明微环与常规水泥的等效声阻抗适当降低,更有利于弯曲型兰姆波传播时与套后介质实现法向刚度的匹配.拉伸波和弯曲型兰姆波对同一胶结状况的不同响应特征也为固井质量综合评价时区分不同的水泥胶结状况提供了可能.

     

Acoustic energy transfer to the upper atmosphere from sinusoidal sources and a role of nonlinear processes

In the framework of solving the problem of acoustic energy transfer from near-surface sources through the upper atmosphere, the propagation of sinusoidal signals of different origin is studied. All calculations are made by means of a model that takes into account the inhomogeneity of the atmosphere, nonlinear effects, absorption, divergence of wave front due to long-range acoustic wave propagation, etc., but does not include the effect of gravity. Infrasonic waves of various periods and their absorption at various heights of the atmosphere are investigated. The calculations show that a sinusoidal signal is destroyed by nonlinear processes during its upward propagation; it transforms into two, initial and final, impulses. The location of the “transformation zone” depends on frequency; its height increases with decreasing frequency. The acoustic waves can heat the upper atmosphere, for example, waves with a period of 3 min generated by thunderstorms can heat the atmosphere by up to ΔT_a=13.08 K/day in the region of 323–431 km. The efficiency of a point artificial emitter is too weak to heat the atmosphere significantly.     

The energy and energy flux of planetary waves in an ocean of variable depth

Abstract

In a recent paper, Buchwald (1972a) has shown that besides the kinetic energy and gravitational potential energy usually associated with planetary waves in an ocean of uniform depth it is useful to define also a “spin energy”, associated with the rotation.

The present paper is basically an extension of Buchwald's result to a uniformly rotating β-plane ocean of variable depth. As in the previous work, energy conservation equations are derived and the separate energies shown to be independently conserved over the total volume of the ocean. The time-averaged energies are further shown to be propagated in the direction of the group velocity and to satisfy the equipartition rule.

Unlike Buchwald, however, we need not consider the boundary conditions in order to achieve these results. Furthermore, the use of a more realistic ocean configuration admits the possibility of a multiply connected region in the present of mean currents.

Finally, there is a physical explanation for the appearance of a spin energy in a rotating system.     

基于黏弹滑移界面理论揭示套管中模式波的传播特征

目前固井质量评价主要是利用套管中模式波的幅度或衰减变化判断套管与水泥间的胶结状况.在超声测量频段（70~500 kHz）,现有声波测井仪器工作时在套管中激发的模式波类似薄板中的对称兰姆波（拉伸波）或反对称兰姆波（弯曲型兰姆波）.本文将黏弹滑移界面理论应用到套管和水泥的耦合界面,探讨了套管中的准兰姆波（包括拉伸波和弯曲型兰姆波）与套管后物质的耦合方式,拉伸波与套后物质主要以剪切刚度耦合,即便是0.01 mm的微环也会使得拉伸波的衰减明显降低,接近套后是流体时的响应特征;而弯曲型兰姆波与套管后物质主要以法向刚度耦合,这使得在套后胶结轻质水泥时弯曲型兰姆波对微环不敏感,在套后耦合常规水泥时微环的存在又会使得弯曲型兰姆波的衰减明显增强,衰减的增加说明其与套后物质的声耦合更紧密,也表明微环与常规水泥的等效声阻抗适当降低,更有利于弯曲型兰姆波传播时与套后介质实现法向刚度的匹配.拉伸波和弯曲型兰姆波对同一胶结状况的不同响应特征也为固井质量综合评价时区分不同的水泥胶结状况提供了可能.     

有限元方法研究精细地-电离层波导VLF波传播特性

基于频域有限元方法仿真了精细地-电离层波导结构甚低频(VLF, Very Low Frequency)电磁波幅度和相位传播特性.首先给出了如何确定VLF波发射点和接收点传播路径所在大圆的方法, 接着分析了获取波导结构中不同阶波导模式传播系数的耦合模理论, 数值讨论了不同阶波导模式的衰减率和相对相速度随模式数和工作频率的变化关系, 给出了波导不同结构参数对一阶模衰减率和相对相速度的影响.与文献结果对比验证了本文有限元方法模拟VLF波传播的正确性和高效性.最后利用实验和数值仿真结果, 通过对电子密度国际电离层参考模型进行修正, 讨论了澳大利亚—青岛台VLF波幅度和相位日变化的规律.本文工作为研究地-电离层波导结构VLF波电磁特性以及提高陆基超远程甚低频导航系统的精度, 提供了新的思路和方法.

     

近日太阳风中磁场回弯结构的MHD模拟

帕克太阳探针(Parker Solar Probe,PSP)在太阳附近发现大量磁力线回弯结构,通常还伴随有太阳风速度增加.这些磁力线回弯的产生机制到目前为止有多种解释,其中有代表性的一种是由慢太阳风中的喷流引起的.我们首先对PSP的就地观测数据进行了统计分析并给出了发生率和空间尺度随径向距离的演化情况,然后使用简化的1.5维磁流体动力学(magnetohydrodynamics,MHD)模型对喷流在太阳风中的演化进行了模拟,其中太阳风被简化为位于黄道面的球对称流.模拟结果表明喷流的确可以导致太阳附近磁力线发生偏转,验证了喷流可以对磁场方向改变有贡献的图景.不过喷流形成的原因还需要进一步研究.

     

Note on the propagation of waves from a spherical cavity in an infinite solid

Summary The present note, as its title implies, is concerned with the investigation of disturbances in an infinite elastic medium containing an initial magnetic field in the axial direction. The equations ofMaxwell, those of elasticity have been effectively made use of to solve the problem.     

Oxygen and water vapor absorption of radio waves in the atmosphere

Summary Calculated values of the gaseous atmospheric absorption are presented for the frequency range 100 to 50,000 Mc at elevations above ground up to at least 130,000 feet, for average conditions during February and August at Bismarck, N. D. and Washington, D. C. Total radio path absorptionsare presented for tropospheric forward scatter communication links for distances of 100, 300 and 1000 miles. The total path absorptions were calculated by summing the absorption contributed by each portion of the atmosphere traversed by a radio ray passing from a 60 foot parabolic antenna resting on the ground to the scattering center and then to a similar receiving antenna. A correlation of total path absorption with the surface value of absolute humidity is developed, thus providing estimates of the range of absorption values in different geographic areas. Maps of average absolute humidity for the world are presented. Previous work on rain absorption is then combined with the present study to provide estimates of the radio power loss due to absorption expected to be exceeded 1 per cent of the time.Portions of this paper were presented in preliminary form at the Symposium on Communication by Scatter Techniques-George Washington University, Washington, D. C., November 14 and 15, 1955.     

Impact of the surface temperature and vertical shear of zonal wind on the dynamics of a simple two-layer model of the atmosphere

The paper presents and analyzes, from the point of view of smooth dynamic systems theory, a two-layer baroclinic model of the troposphere in geostrophic approximation. The model describes airflow in β-channel within the tropospheric part of the main Hadley circulation cell. It enables to obtain, after application of the Galerkin method, a fairly simple low-parametric dynamic system describing the phenomena of non-linear interactions, bifurcations and blocking in the atmosphere. This enables to take into consideration such basic factors influencing the atmospheric dynamics like the heat exchange within the surface, orography, vertical variability of zonal wind and hydrostatic stability. Impact of zonal thermal variability of the surface and vertical shear of zonal wind in the troposphere on the orographic bifurcation was investigated and the oscillation character in the dynamic system after Hopf bifurcation of the second kind was analyzed. Additionally, the model dynamics was investigated in conditions including momentum forcing in the upper and lower parts of the troposphere and excluding orographic interaction, as well as in the conditions of thermal interaction between the troposphere and the surface for the vertical shear of zonal wind in both tropospheric layers. Impact of the mean zonal wind in the troposphere on the properties of model dynamics was assessed. It was proved that zonally varied surface temperature and layered mean zonal wind in the atmosphere are the parameters that have basic influence on the model dynamics. They cause numerous bifurcations and strongly influence the periods of oscillations of the model variables. They are often Hopf bifurcations of the second kind during which tropospheric states fairly distant from the ones before the bifurcations are generated. This significantly influences the model predictability.     

Radiosonde observations of high-latitude planetary waves in the lower atmosphere

The characteristics of high-latitude planetary waves (PWs) in the troposphere and lower stratosphere (TLS) are studied by using the data from radiosonde observations during 1998 to 2006 at three Alaskan stations in USA (Nome, 64.50°N, 165.43°W; McGrath, 62.97°N, 155.62°W; Fairbanks, 64.82°N, 147.87°W). It is found that strong PWs exist in two regions. One is around tropopause, and the other is in the polar night jet (PNJ) in winter. The PW activities are rather intermittent, and their lifetimes are no longe...     

大气湍流能谱的精细结构及能量级串

利用小波变换和傅里叶分析对近地层大气湍流脉动资料进行了分析,发现波数空间能谱著名 的“-5/3”标度律成立的区间中存在突变点;还发现对应于小波变换时间尺度2j,j=1, 2,…,j0,高频分量按照2(j-2)-1(j>1)的方式级串,这符合同步级串的物理图象 ;在标度区间内高频分量作用于幂律局部特征的效果是平均的,不存在影响标度指数的特征 频谱. 利用不同高度大气湍流资料和不同小波基函数作变换,结果是一致的. 我们还对H= 1/3的分形布朗运动产生的随机序列进行了对比实验,发现从能谱角度,实际发达大气湍流 偏离高斯分布的程度很小,二者的差别只在高阶标度律时明显. 