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151.
SOHO/UVCS data indicate that minor ions in the corona are heated more than hydrogen, and that coronal heating results in T⊥ larger than T‖. Analogous behavior has been known from in situ measurements in solar wind for many years. Here we compare and contrast two
mechanisms which have been proposed to account for the above behavior: ion-cyclotron resonance and gravity damping.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
152.
Michael R. Collier Aaron Roberts Adolfo Viñas 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(10):1704-1709
We describe a new wave mode similar to the acoustic wave in which both density and velocity fluctuate. Unlike the acoustic wave in which the underlying distribution is Maxwellian, this new wave mode occurs when the underlying distribution is a suprathermal κ-function and involves fluctuations in the power law index, κ. This wave mode always propagates faster than the acoustic wave with an equivalent effective temperature and becomes the acoustic wave in the Maxwellian limit as κ → ∞. 相似文献
153.
The review contains the important achievements in dynamics of the galactic disks. Among them there are I. New structures
discovered recently: • giant vortices (including giant anticyclone in the Solar vicinity); • slow bar; • inner oscillating
structure within spiral arms similar that of enveloped soliton; • chaotic streamlines in the velocity field of the gaseous
disk of a real galaxy. II. New collective phenomina discovered recently: • new overreflection instability initiating ‘mini-spiral’
in the innermost central parsec of Galaxy; • large-scale convection caused by nonlinear interaction of density wave with
disk gas; • non-kolmogorovian spectrum of weak turbulence corresponding to the observed one in the • Solar vicinity. III. New
methods worked out recently: • reconstruction of full three-dimensional vector field of gas velocity from the observed line-of-
• sight velocity field; • observational test for verification of the wave-nature of the spiral arms; • observational test
to distinguish two types of vertical motions: warp and z-motions in the • density wave; • derivation of correct system of two-dimensional dynamical equations from the initial three-
• dimensional one.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
154.
通过对用于脉冲爆震引燃的内楔表面激波聚焦冷态流场的数值模拟,分析了不同角度内楔表面在激波聚焦时流场结构的不同特点。数值计算的结果表明:对于大内楔角的情况,激波进入内楔角之后产生规则反射,温度的大幅度升高发生在激波于内楔顶点反射之后;对于小内楔角的情况,激波进入内楔角之后产生马赫反射,温度的升高在入射激波到达内楔顶点之前就已经发生,而在入射激波于内楔顶点反射之后得到进一步的提升。同时,还对不同角度内楔的反射激波后气流温度进行了比较。 相似文献
155.
156.
基于带化学反应的二维轴对称Eu ler方程,利用带限制函数的波传播算法,在两端均敞开和一端封闭一端敞开的两种边界情况下,对圆柱型燃烧室中的氢气-空气预混气的聚心燃烧进行了数值模拟,探讨了聚心火焰引发爆轰过程中的波系结构以及火焰的变形。数值结果表明,在两端均敞开的情况下,燃烧诱导的激波在轴心、火焰和壁面之间来回反射,使火焰失稳,加速了火焰的燃烧,但没有转变成爆轰。而在一端封闭的情况下,封闭端反射产生的激波,不断穿越火焰,使火焰严重失稳,加剧了燃烧速度,最终导致爆轰的形成。稳定爆轰阵面的参数与CJ理论计算的结果进行了对比,两者符合的较好。同时,火焰在与激波的作用过程中,形状扭曲变形,对于两端敞开的情况呈对称的扁平头部蘑菇云,而对于一端封闭的情况,则呈封闭端小敞口端大的扁平头部蘑菇云。 相似文献
157.
为研究超声速燃烧和爆轰相关的机理问题,提出了一种结合燃烧型加热器和阵列喷管的超声速预混加热器设计思想。通过预热燃烧室来提供总温可变的高焓富氧气流,经过特征线型面喷管膨胀降温后,在喷管扩张段的适当位置以一定角度喷入燃料,经过混合段后形成所需的连续高焓总温和当量比可调的预混气流。通过对混合过程的数值模拟和预混气体的着火延迟时间分析了当前的预混高焓加热器的混合和自燃问题。在超声速气流中加入斜劈采用纹影技术进行激波点火实验,并验证了当前的预混加热器设计是成功。 相似文献
158.
K. Andreov L. Pech 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2007,40(12):1871-1880
This paper is devoted to the study of propagation of disturbances caused by interplanetary shocks (IPS) through the Earth’s magnetosphere. Using simultaneous observations of various fast forward shocks by different satellites in the solar wind, magnetosheath and magnetosphere from 1995 till 2002, we traced the interplanetary shocks into the Earth’s magnetosphere, we calculated the velocity of their propagation into the Earth’s magnetosphere and analyzed fronts of the disturbances. From the onset of disturbances at different satellites in the magnetosphere we obtained speed values ranging from 500 to 1300 km/s in the direction along the IP shock normal, that is in a general agreement with results of previous numerical MHD simulations. The paper discusses in detail a sequence of two events on November 9th, 2002. For the two cases we estimated the propagation speed of the IP shock caused disturbance between the dayside and nightside magnetosphere to be 590 km/s and 714–741 km/s, respectively. We partially attributed this increase to higher Alfven speed in the outer magnetosphere due to the compression of the magnetosphere as a consequence of the first event, and partially to the faster and stronger driving interplanetary shock. High-time resolution GOES magnetic field data revealed a complex structure of the compressional wave fronts at the dayside geosynchronous orbit during these events, with initial very steep parts (10 s). We discuss a few possible mechanisms of such steep front formation in the paper. 相似文献
159.
160.
A. Guglielmi J. Kangas J. Kultima A. Potapov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2005,36(12):2413-2416
There are a host of factors influencing the excitation of Pc1 geomagnetic pulsations, which are ULF waves in the frequency range between 0.2 and 5 Hz. We have studied carefully the dependence of the pearl-type Pc1 activity at Sodankylä, Finland (L = 5.1) on the plasma density N in front of the magnetosphere, the bulk velocity V of the solar wind, and the intensity B of the IMF. The result is as follows: high values of N and reduced values of V are favorable to appearance of Pc1, whereas the dependence of Pc1 activity on B is practically absent. We also show that the probability of Pc1 occurrence decreases with the interplanetary electric field, and increases with solar wind impact pressure and with the plasma to magnetic pressure ratio “beta”. 相似文献