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11.
D.R. Japaridze M.Sh. Gigolashvili V.J. Kukhianidze 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2007,40(12):1912-1916
The differential rotation of the patterns of the large-scale solar magnetic field during solar activity cycles 20 and 21 is investigated. Compact magnetic elements with the polarity of the general solar magnetic field have larger speed of rotation than the elements with the opposite polarity. The surface of the Sun was divided by 10°-zones. In all of them the average rotation rate of the magnetic elements with negative polarity is little higher than that of the magnetic elements with positive polarity, except for 50°-zone of the south hemisphere and at the 10° latitude of the north hemisphere.
The rates of differential rotation for large-scale magnetic elements with negative and positive polarities have similar behavior for both cycles of the solar activity.
The rotation rate varies at polarity reversal of the circumpolar magnetic fields. For the cycle No 20 in 1969–1970 the threefold reversal took place in the northern hemisphere and variations of rotation rate can be noticed for magnetic elements both with positive and negative polarity for each 10°-zone in the same hemisphere. 相似文献
12.
Martin A. Lee 《Space Science Reviews》2007,130(1-4):221-229
Gradual solar energetic particle (SEP) events are evidently accelerated by coronal/interplanetary shocks driven by coronal
mass ejections. This talk addresses the different factors which determine the composition of the accelerated ions. The first
factor is the set of available seed populations including the solar wind core and suprathermal tail, remnant impulsive events
from preceding solar flares, and remnant gradual events. The second factor is the fractionation of the seed ions by the injection
process, that is, what fraction of the ions are extracted by the shock to participate in diffusive shock acceleration. Injection
is a controversial topic since it depends on the detailed electromagnetic structure of the shock transition and the transport
of ions in these structured fields, both of which are not well understood or determined theoretically. The third factor is
fractionation during the acceleration process, due to the dependence of ion transport in the turbulent electromagnetic fields
adjacent to the shock on the mass/charge ratio. Of crucial importance in the last two factors is the magnetic obliquity of
the shock. The form of the proton-excited hydromagnetic wave spectrum is also important. Finally, more subtle effects on ion
composition arise from the superposition of ion contributions over the time history of the shock along the observer’s magnetic
flux tube, and the sequence of flux tubes sampled by the observer. 相似文献
13.
空间能量粒子探测方法研究 总被引:1,自引:0,他引:1
阐述了空间能量粒子探测的原理和方法。介绍了国外在能量粒子探测方面所采用的半导体望远镜测量法、电场加速法、磁偏转法等方法,分析了它们各自的优缺点。就制约能量粒子探测技术发展的关键因素进行了讨论。并以此为基础,结合我国实际情况提出了一种新的探测方法。 相似文献
14.
H. J. Völk 《Space Science Reviews》2007,130(1-4):431-438
The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient
of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce
the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of
Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount
of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar
initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic
Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in
the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming
from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×1018 eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall
Cosmic Ray spectrum. 相似文献
15.
A.G. Lyne 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2006,38(12):2716-2720
A recent multibeam pulsar survey of the outer Galactic plane at Parkes has discovered the first-known double-pulsar binary, a very compact double neutron star system in which both stars are observable as radio pulsars. In this review, we briefly describe the discovery and the studies which have been enabled by the unique properties of the system. These range from the most precise confirmation yet of the theory of general relativity, with the possibility of even more new tests and the measurement of second-order post-Newtonian effects, to studies of the magnetospheres and emission properties of the two pulsars. The discovery also results in a significant increase in the expected rate of occurrence of the mergers of double neutron star systems, and hence the rate of detection of such events by the new ground-based gravitational wave detectors. 相似文献
16.
The Bastille-day event in 2000 produced energetic 3B/X5.6 flare with a halo CME, which had great geo-effects consequently.
This event has been studied extensively and it is considered that it follows the two-ribbon flare model. The flare/CME event
was triggered by an erupting filament and TRACE observations showed formation of giant arcade structures during the flare
process. Hard X-ray (HXR) two ribbons revealed for the first time in this flare event (Masuda et al., 2001). The reconstruction of 3-D coronal magnetic fields revealed a magnetic flux rope structure, for the first time, from
extrapolation of observed photospheric vector magnetogram data and the flux rope structure was co-spatial with portion of
the filament and a UV bright lane (Yan et al., 2001a, 2001b). Here we review some recent work related to the flux rope structure and the HXR two ribbons by comparing their
locations and the flux temporal profiles during the flare process so as to understand the energy release and particle accelerations.
It is proposed that the rope instability may have triggered the flare event, and reconnection may occur during this process.
The drifting pulsation structure in the decimetric frequency range is considered to manifest the rope ejection, or the initial
phase of the coronal mass ejection. The HXR two ribbons were distributed along the flux rope and the rope foot points coincide
with HXR sources. The energy dissipation from IPS observations occurred within about 100 R
⋅ is consistent with the estimate for the flux rope system.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
17.
本文介绍用 Visual FoxPro的定时器。标签、按钮等控件和控件的属性、方法、事件等在界面上设计动态字幕、动态按钮等若干动态效果的方法。 相似文献
18.
19.
在引入了一套磨粒形态学描述子来提取磨损颗粒的显微形态特征的基础上 ,采用人工神经网络技术 ,编制了用于磨损颗粒自动识别的 BP网络计算机模拟程序。在网络训练的过程中应用了本文引入的因子模糊化训练方法 ,使训练速度大大加快 ,以异或问题为例 ,速度可提高 5~ 1 0倍。应用此网络对磨粒测试库进行识别实验 ,识别正确率在 90 %以上 ,并且识别速度很快 ,大大优于传统的磨粒识别方法。 相似文献
20.
研究了稀土加入三种电沉积镍基复合镀层Ni—B_4C、Ni—TiC、Ni—ZrO_2前后,在850℃时的氧化行为。通过金相观察、ESCA(光电子能谱)分析及X射线衍射等方法研究表明:镀层中不同的复合颗粒和稀土两者对镀层的抗氧化能力均有影响。其小不同种类的颗粒对镀层抗氧化能力所产生影响的差别很明显;而稀土对镀层抗氧化能力影响的差别较小,且影响的程度比较接近。另外,两者影响的机理也不同。颗粒是通过分解、扩散等过程改变表面膜的组成来影响的,而稀土则是从提高膜的致密度和膜与基体的粘附性来影响的。作者认为,它们的影响既互相独立,而又互相补充。 相似文献