共查询到20条相似文献，搜索用时 15 毫秒
1.
本文统计了第２２ 太阳活动周期间（１９９１ ～１９９５ 年） 发生的２５ 个太阳质子事件与太阳耀斑及日冕物质抛射（ＣＭＥ） 事件的关系 统计结果表明, 所有的太阳质子事件都与耀斑发生相关, 除２ 个质子事件（１９９４１０２０ 和１９９５１０２０ 日发生的太阳质子事件） 与ＣＭＥ发生无关, 其余质子事件也都与ＣＭＥ 相关 值得注意的是, 与质子事件相关的耀斑有１６ 个是双带耀斑, 其中包括与ＣＭＥ无关的２ 个事件的耀斑, 占总数的６４ ％ 上述统计结果证实了无论是太阳耀斑, 还是物质抛射, 它们对太阳质子事件的发生同样起着非常重要的作用 相似文献
2.
Observational connection between local high-temperature phenomena within magnetic clouds and the Sun
Magnetic clouds (MCs) frequently show abnormal high-ionization states of heavy ions. The abnormal high-charge distributions are related to the coronal temperature of their source regions. We examined the plasma and magnetic field data of 74 MCs observed by the Advanced Composition Explorer from February 1998 to December 2008. We determined that 14 of the 74 events showed local high-temperature phenomena. We analyzed the correlation between proton temperature and O7/O6 ratio (or high mean Fe charge state 〈Fe〉) within the local high-temperature regions in the 14 MCs. Results show that proton temperature and O7/O6 ratio (or high mean Fe charge state) had good correlations in nine MCs, but had no evident correlation in the other five MCs. The local high-temperature phenomena within the nine MCs have resulted from the Sun. 相似文献
3.
使用二维粒子模拟（PIC）的方法研究了在电流片两侧具有不同温度或密度情况下的无碰撞磁场重联过程.在初始等离子体密度非对称的情况下,发现重联区等离子体流场结构、电磁场结构以及重联过程与对称情况下的结果有明显不同.通过对电流片两侧温度比取不同的参数Tm/Ts=1,2,5进行模拟(其中Tm和Ts分别代表磁层侧和磁鞘侧的温度),结果分析发现,(1)在密度非对称系统中,出流区电子沿着分离面出现一个整体的从高密度区向低密度区的流动,并围绕磁岛形成一个电流环;(2)在高温低密度一侧,在重联过程中,分离面两侧将出现很强的电荷分离并产生一个基本垂直于分离面的强度较大的电场Ez,其幅度和空间尺度与温度梯度近似地成线性正比和反比关系.在初始电流片两侧温度之比取Tm/Ts=5的情况下,Ez的幅度将达到0.71,其空间尺度与局地电子惯性长度de同一量级,这一结果与观测相吻合;(3)重联率随着温度梯度增大而下降. 相似文献
4.
A program for identifying magnetic clouds in patrol satellite data, which recorded the interplanetary medium parameters near
the magnetosphere, has been developed based on the cloud model in the form of a force-free cylindrical flux tube. The program
makes it possible to also determine the entire magnetic field distribution in a cloud that approaches the Earth, using the
initial satellite measurements. For this purpose, a model cloud (which has the maximal correlation coefficient with an analyzed
cloud with respect to three magnetic field vector components and minimal rms deviations of the magnetic field and velocity
components) is selected from the preliminarily created database including 2 million model clouds. The obtained magnetic field
distribution in a cloud will make it possible to predict the intensity of a magnetic storm that this cloud will cause. 相似文献
5.
M. A. Livshits 《Geomagnetism and Aeronomy》2009,49(8):1069-1071
Data on high-energy processes on the Sun are summarized. We refine the classification of flares and substantiate the view
that a coronal mass ejection and a flare proper are manifestations of the same common process, at least for the most powerful
events. Next, we analyze data on the acceleration of electrons (RHESSI, Mars Odyssey) and protons. The existence of two peaks
of hard X-ray emission spaced 10–20 min apart and the evolution of its spectra are shown to be indicative of two acceleration
episodes. We have analyzed the spectra of 172 proton increases identified with the ratio of the proton fluxes at energies
above 10 and 100 MeV near the Earth. These spectra turn out to be virtually the same for most of the large flares under favorable
conditions for the escape of particles from the corona and their propagation in the interplanetary space. This is an argument
for the invariance of the main features of efficient particle acceleration in powerful events. This process takes place at
the explosive phase of a flare and its source is located low, immediately above the chromosphere, in the region adjacent to
sunspots. There is a reason to believe that, in this case, a rapid simultaneous acceleration of electrons and protons takes
place with the capture of some fraction of the particles into magnetic traps. However, there exist a few events in which an
additional number of protons with energies as high as 10–30 MeV escape from the corona at the post-eruptive phase of flare
development. Analysis of these cases with softer particle spectra more likely suggests an additional particle acceleration
at coronal heights (about 30 000 km) than the facilitation of particle escape from magnetic traps. We estimate the contribution
from the proton flux at an energy above 10 MeV arising at the post-eruptive phase of a flare to the total particle flux at
the maximum of a proton increase and discuss possible particle acceleration mechanisms at significant coronal heights. 相似文献
6.
Early in 1996, the latest of the European inco-herent-scatter (EISCAT) radars came into operation on the Svalbard islands. The EISCAT Svalbard Radar (ESR) has been built in order to study the ionosphere in the northern polar cap and in particular, the dayside cusp. Conditions in the upper atmosphere in the cusp region are complex, with magnetosheath plasma cascading freely into the atmosphere along open magnetic field lines as a result of magnetic reconnection at the dayside magnetopause. A model has been developed to predict the effects of pulsed reconnection and the subsequent cusp precipitation in the ionosphere. Using this model we have successfully recreated some of the major features seen in photometer and satellite data within the cusp. In this paper, the work is extended to predict the signatures of pulsed reconnection in ESR data when the radar is pointed along the magnetic field. It is expected that enhancements in both electron concentration and electron temperature will be observed. Whether these enhancements are continuous in time or occur as a series of separate events is shown to depend critically on where the open/closed field-line boundary is with respect to the radar. This is shown to be particularly true when reconnection pulses are superposed on a steady background rate. 相似文献
7.
在2001～2003年Cluster飞船通过近地磁尾期间,共探测到14次重联事件,在这些事件中同时还观测到等离子体波活动.本文把14次事件分为三大类,其中：第I类包含了8次事件,它们是在等离子体片内先于重联事件观测到波活动,并且还同时观测到Hall磁场.经过分析判断,这类事件中观测到的波是右旋偏振的哨声波.第II类包含了2次事件,这类事件也观测到了Hall磁场和右旋偏振的哨声波.第Ⅲ类也包含了2次事件,这类事件只是普通的重联事件,没有观测到Hall磁场,但是波活动明显先于重联事件.在我们观测的14次事件中,比较强烈的哨声波和Hall 磁场是一一对应的,因此哨声波可能主要是在Hall磁场的四极结构区激发的. 相似文献
8.
Experimental proofs of the existence of the formation and destruction mechanisms of solar proton belts in the inner magnetosphere at a rapid change in the penetration boundary of solar protons are presented. An analysis of the measurements of solar protons and alpha-particles on board the Coronas-F low-altitude polar satellite during the magnetic storms in October–November 2003 is performed. During this period, formation and destruction of the belts of solar cosmic rays was observed several times. The compression of the magnetosphere during a storm makes possible the direct penetration of solar protons deep into the inner magnetosphere. The proton trajectories outside the penetration boundary are open, and the preliminary captured particles can easily leave the magnetosphere. During the recovery of the magnetospheric configuration, when the penetration boundary goes away from the Earth, the solar protons and alpha-particles with relatively low velocity of the magnetic drift remain stably captured, whereas the particles of higher energies follow the motion of the penetration boundary. That is why the energy range of the captured protons is limited from above in contrast to the effect of injection during ineffective SC in the low-energy region. 相似文献
9.
The open magnetosphere model of cusp ion injection, acceleration and precipitation is used to predict the dispersion characteristics for fully pulsed magnetic reconnection at a low-latitude magnetopause X-line. The resulting steps, as would be seen by a satellite moving meridionally and normal to the ionospheric projection of the X-line, are compared with those seen by satellites moving longitudinally, along the open/closed boundary. It is shown that two observed cases can be explained by similar magnetosheath and reconnection characteristics, and that the major differences between them are well explained by the different satellite paths through the events. Both cases were observed in association with poleward-moving transient events seen by ground-based radar, as also predicted by the theory. The results show that the reconnection is pulsed but strongly imply it cannot also be spatially patchy, in the sense of isolated X-lines which independently are intermittently active. Furthermore they show that the reconnection pulses responsible for the poleward-moving events and the cusp ion steps, must cover at least 3 h of magnetic local time, although propagation of the active reconnection region may mean that it does not extend this far at any one instant of time. 相似文献
10.
B. Strauss R. Meerkoetter B. Wissinger P. Wendling M. Hess 《Annales Geophysicae》1997,15(11):1457-1467
The impact of contrail-induced cirrus clouds on regional climate is estimated for mean atmospheric conditions of southern Germany in the months of July and October. This is done by use of a regionalized one-dimensional radiative convective model (RCM). The influence of an increased ice cloud cover is studied by comparing RCM results representing climatological values with a modified case. In order to study the sensitivity of this effect on the radiative characteristics of the ice cloud, two types of additional ice clouds were modelled: cirrus and contrails, the latter cloud type containing a higher number of smaller and less of the larger cloud particles. Ice cloud parameters are calculated on the basis of a particle size distribution which covers the range from 2 to 2000 m, taking into consideration recent measurements which show a remarkable amount of particles smaller than 20 m. It turns out that a 10% increase in ice cloud cover leads to a surface temperature increase in the order of 1K, ranging from 1.1 to 1.2K in July and from 0.8 to 0.9K in October depending on the radiative characteristics of the air-traffic-induced ice clouds. Modelling the current contrail cloud cover which is near 0.5% over Europe yields a surface temperature increase in the order of 0.05 K. 相似文献
11.
12.
《Journal of Atmospheric and Solar》2000,62(10):833-849
We present Interball Tail Probe observations from the high latitude mid-tail magnetopause which provide evidence of reconnection between the interplanetary magnetic field (IMF) and lobe field lines during a 6 h interval of stable northward and dawnward IMF on October 19, 1995. Results from a global magnetohydrodynamic simulation for this interval compare well with the Interball observations. With the simulations, we provide an extended global view of this event which gives us insight into the reconnection and convection dynamics of the magnetosphere. We find that reconnection occurs in a region of limited spatial extent near the terminator and where the IMF and the lobe field are anti-parallel. Reconnected IMF field lines drape over the dayside magnetosphere, convect along the flanks into the nightside, and enter the magnetotail through a small entry window that is located in the flank opposite to the reconnection site. Ionospheric convection is consistent with previous observations under similar IMF conditions and exhibits a two cell pattern with a dominant lobe cell over the pole. The magnetic mapping between the ionosphere and the lobe boundary is characterized by two singularities: the narrow entry window in the tail maps to a 6 h wide section of the ionospheric lobe cell. A singular mapping line cuts the lobe cell open and maps to almost the entire tail magnetopause. By this singularity the magnetosphere avoids having a stagnation point, i.e., the lobe cell center maps to a tailward convecting field line. The existence of singularities in the magnetic mapping between the ionosphere and the tail has important implications for the study of tail–ionosphere coupling via empirical magnetic field models. Because the lobe–IMF reconnection cuts away old lobe flux and replaces it with flux tubes of magnetosheath origin, solar wind plasma enters the lobes in a process that is similar to the one that operates during southward IMF. 相似文献
13.
The cause-and-effect relations of the dynamics of high-latitude geomagnetic activity (in terms of the AL index) and the type of the magnetic cloud of the solar wind are studied with the use of artificial neural networks. A recurrent neural network model has been created based on the search for the optimal physically coupled input and output parameters characterizing the action of a plasma flux belonging to a certain magnetic cloud type on the magnetosphere. It has been shown that, with IMF components as input parameters of neural networks with allowance for a 90-min prehistory, it is possible to retrieve the AL sequence with an accuracy to ~80%. The successful retrieval of the AL dynamics by the used data indicates the presence of a close nonlinear connection of the AL index with cloud parameters. The created neural network models can be applied with high efficiency to retrieve the AL index, both in periods of isolated magnetospheric substorms and in periods of the interaction between the Earth’s magnetosphere and magnetic clouds of different types. The developed model of AL index retrieval can be used to detect magnetic clouds. 相似文献
14.
《Journal of Atmospheric and Solar》2000,62(9):737-749
During an interaction of the Earth’s magnetosphere with the interplanetary magnetic cloud on October 18–19, 1995, a great magnetic storm took place. Extremely intense disturbances of the geomagnetic field and ionosphere were recorded at the midlatitude observatory at Irkutsk (Φ′≈45°, Λ′≈177°, L≈2) in the course of the storm. The most important storm features in the ionosphere and magnetic field are: a significant decrease in the geomagnetic field Z component during the storm main phase; unusually large amplitudes of geomagnetic pulsations in the Pi1 frequency band; extremely low values of critical frequencies of the ionospheric F2-layer; an appearance of intense Es-layers similar to auroral sporadic layers at the end of the recovery phase. These magnetic storm manifestations are typical for auroral and subauroral latitudes but are extremely rare in middle latitudes. We analyze the storm-time midlatitude phenomena and attempt to explore the magnetospheric storm processes using the data of ground observations of geomagnetic pulsations. It is concluded that the dominant mechanism responsible for the development of the October 18–19, 1995 storm is the quasi-stationary transport of plasma sheet particles up to L≈2 shells rather than multiple substorm injections of plasma clouds into the inner magnetosphere. 相似文献
15.
The results of a three-dimensional MHD simulation and data obtained using specialized spacecraft made it possible to construct
an electrodynamic model of solar flares. A flare results from explosive magnetic reconnection in a current sheet above an
active region, and electrons accelerated in field-aligned currents cause hard X rays on the solar surface. In this review,
we considered works where the boundary and initial conditions on the photosphere were specified directly from the magnetic
maps, obtained by SOHO MDI in the preflare state, in order to simulate the formation of a current sheet. A numerical solution
of the complete set of MHD equations, performed using the new-generation PERESVET program, demonstrated the formation of several
current sheets before a series of flares. A comparison of the observed relativistic proton spectra and the simulated proton
acceleration along a magnetic field singular line made it possible to estimate the magnetic reconnection rate during a flare
(∼107 cm s−1). Great flares (of the X class) originate after an increase in the active region magnetic flux up to 1022 Mx. 相似文献
16.
应用二维磁流体动力学模拟方法数值研究了三层电流片中电阻撕裂模不稳定性的特征及磁场重联过程．结果表明，这是一种复杂的非稳态磁场重联．在初期阶段，三个电流片中分别由撕裂模不稳定性引起磁场重联，形成薄而长的磁岛．随着撕裂模不稳定性的非线性发展，每个磁岛的宽度都逐步增大，以至导致新的磁场重联发生．同时，三个电流片的强度都逐渐减弱，且原中心反向电流区最终消失．部分磁能不断地转化为等离子体的热能和动能，引起等离子体的加热和加速．多层电流片中撕裂模不稳定性引起的自发重联，可能对太阳耀斑、日冕加热、太阳风与磁层耦合等有重要影响． 相似文献
17.
We consider the prolonged injection of the high-energy (> 10 MeV) protons during the three successive events observed by GOES in October 1989. We apply a solar-rotation-stereoscopy approach to study the injection of the accelerated particles from the CME-driven interplanetary shock waves in order to find out how the effectiveness of the particle acceleration and/or escape depends on the angular distance from the shock axis. We use an empirical model for the proton injection at the shock and a standard model of the interplanetary transport. The model can reproduce rather well the observed intensity-time profiles of the October 1989 events. The deduced proton injection rate is highest at the nose of the shock; the injection spectrum is always harder near the Sun. The results seem to be consistent with the scheme that the CME-driven interplanetary shock waves accelerate a seed particle population of coronal origin. 相似文献
18.
19.
M.A. Hidalgo J.J. Blanco F.J. Alvarez T. Nieves-Chinchilla 《Journal of Atmospheric and Solar》2011,73(11-12):1372-1379
The fact that magnetic clouds are one of the main sources causing geomagnetic storms is a well-established fact. One of the issues is to establish those features of magnetic clouds determinant in the intensity of the Dst corresponding to geomagnetic storms. We examine measurements of geoeffective magnetic clouds during the period 1995–2006 providing geomagnetic storms with Dst indexes lower than ?100 nT. These involve 46 geomagnetic storm events. After establishing the different characteristics of the magnetic clouds (plasma velocity, maximum magnetic intensity, etc.) we show some results about the correlations found among them and the storms intensity, finding that maximum magnetic field magnitude is a determinant factor to establish the importance of magnetic clouds in generating geomagnetic storms, having a correlation as good as the electric convective field. 相似文献