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1.
A simple diffusion model of Saturn's radiation belts with a constant internal source and particle losses at the boundaries is considered. The radial diffusion coefficient is supposed to be D
LL L
4. The analytical solution to the stationary diffusion equation describes well the observed radial profiles of the distribution function of energetic protons in Saturn's magnetosphere. 相似文献
2.
In 1964, during flights of the ELECTRON satellites the narrow belts of energetic electrons (E
e ≈ 6MeV) have been discovered in the Earth’s magnetosphere at L ≈ 2.75. The same structures approximately at the same magnetic shells were found in 2004 by the CORONAS-F and SERVIS-1 satellites. A comparison of the results of these experiments is presented. It is shown that the additional narrow belts of
energetic electrons occur after intense magnetic storms (D
st
> 100 nT), in our cases, having a double-triple structure. The lifetime of these belts is a few months and their disappearance
had a gradual character. The obtained results separated in time by 40 years suggest the constancy of the sources of particles
of the Earth’s radiation belts and processes occurring in the magnetosphere, which ensures not only existence of the radiation
belts, but also the recurrence of various exotic phenomena in the belts similar to the belt of energetic electrons at the
inner magnetic shells. 相似文献
3.
During strong magnetic storms in July and November of 2004 the fluxes of trapped particles (protons and electrons of MeV energies)
in the Earth’s radiation belts have increased by orders of magnitude and then decreased remaining on an enhanced level for
several months. These enhancements allowed us to study the processes of relaxation of the radiation belts. Measurements of
energetic particles by low-altitude satellites Coronas-F and Servis-1 have shown that predictions of the theory about the rate of pitch-angle diffusion are not always correct, giving both overestimated
and underestimated values for the lifetime of energetic particles. 相似文献
4.
A comparative analysis has been carried out of the parameters of energetic electrons in the tail of the Earth’s magnetosphere that belong to three sources, i.e., electrons of solar origin, electrons generated in the magnetosphere of Jupiter, and electrons in the Earth’s magnetosphere. The differences in the time profiles of fluxes and energy spectra of the three electron sources, their relation to fluxes outside the magnetosphere, and periods of the occurrence of electron fluxes of each type are considered. 相似文献
5.
An analysis of enhancements in the fluxes of electrons with energies above 300 keV registered onboard of the Coronas-F satellite in the polar regions at the boundary of the outer radiation belt is performed. Cases are revealed when the increases
in question were observed consequently during multiple crossings of the outer radiation belt boundary. Localization of the
revealed events relative to the auroral oval using the data of almost simultaneous observations of electrons with energies
of 0.1–10 keV on the Meteor-3M satellite and OVATION model is studied. It is shown that almost all studied increases in relativistic electrons are localized
at latitudes of the auroral oval. Various mechanisms which could cause the observed increases are discussed, as well as a
possibility of formation of local traps of energetic particles in the high-latitude magnetosphere. 相似文献
6.
Space charge sheath formation in a magnetized plasma flow around space bodies is considered for the cases of high surface conductivity, free electron emission, dipole magnetic field. The results are applied to explain different phenomena in the ionosphere and magnetosphere of the Earth and planets such as polar aurora and kilometric radiation of the Earth and decametric radiation of the Jovian satellite Io. 相似文献
7.
M. I. Panasyuk M. V. Podzolko A. S. Kovtyukh I. A. Brilkov N. A. Vlasova V. V. Kalegaev V. I. Osedlo V. I. Tulupov I. V. Yashin 《Cosmic Research》2017,55(2):79-87
The Earth’s radiation belts discovered at the end of the 1950s have great scientific and practical interest. Their main characteristics in magnetically quiet periods are well known. However, the dynamics of the Earth’s radiation belts during magnetic storms and substorms, particularly the dynamics of relativistic electrons of the outer belt, when Earth’s radiation belt particle fluxes undergo significant time variations, is studied insufficiently. At present, principally new experiments have been performed and planned with the intention to better study the dynamics of the Earth’s radiation belts and to operationally control the space-energy distributions of the Earth’s radiation belt particle fluxes. In this paper, for spacecraft designed to measure the fluxes of electrons and protons of the Earth’s radiation belts at altitudes of 0.5–10000 km, the optimal versions for detector orientation and orbital parameters have been considered and selected. 相似文献
8.
The local radiation belts of the Sun are defined as giant quasi-stationary coronal and heliospheric traps for solar cosmic rays. These traps are formed by loop magnetic fields, both solar and interplanetary. Using observational data, some experimental examples of the local radiation belts of the Sun are considered. The hypotheses on the origin of energetic particles in the outer heliosphere and on the local radiation belts of the Sun are discussed. 相似文献
9.
Vlasova N. A. Kovtyukh A. S. Kutuzov Yu. V. Mar'in B. V. Pavlov N. N. Rubinshtein I. A. Sosnovets E. N. Teltsov M. V. 《Cosmic Research》2001,39(3):236-245
The dynamics of near plasma sheet electrons and ions (E 0.1–12.4 keV), ring current protons (E
i 41–133 keV), and energetic electrons from the Earth's radiation belts (E
e 97–1010 keV) is considered using the data from the Gorizont-34and Gorizont-35geosynchronous satellites from March 11–25, 1992. Peculiarities of this period are a long (more than 4 days) interval of the northward interplanetary magnetic field (B
z> 0) and a high-speed stream of the solar wind with an enhanced particle density. The SC and compression of the magnetosphere to the geosynchronous orbit (GMC) preceded this interval. Under quiet and moderately disturbed geomagnetic conditions and under a prolonged northward interplanetary magnetic field, we observed a significant decrease of fluxes and softening of spectra of the electron component of plasma in the energy ranges of 0.1–12.4 keV and 97–1010 keV, and of the ion component of plasma at energies of 0.1–4 keV, while the intensity of 5–12.4 keV ion fluxes increases by about one order of magnitude. The peculiarities of distributions of energetic particle fluxes observed in the period under consideration can be associated with significant variations of the convection conditions and a decreased or fully suppressed injection of energetic electrons into the geosynchronous orbit region. 相似文献
10.
Cosmic Research - A distinctive feature of the Jovian magnetosphere is a powerful disklike current system—the current disk. There are several models of the magnetic field of this current... 相似文献
11.
We have considered variations in fields and particle fluxes in the near-Earth plasma sheet on the THEMIS-D satellite together with the auroral dynamics in the satellite-conjugate ionospheric part during two substorm activations on December 19, 2014 with K p = 2. The satellite was at ~8.5RE and MLT = 21.8 in the outer region of captured energetic particles with isotropic ion fluxes near the convection boundary of electrons with an energy of ~10 keV. During substorm activations, the satellite recorded energetic particle injections and magnetic field oscillations with a period of ~90 s. In the satellite-conjugate ionospheric part, the activations were preceded by wavelike disturbances of auroral brightness along the southern azimuthal arc. In the expansion phase of activations, large-scale vortex structures appeared in the structure of auroras. The sudden enhancements of auroral activity (brightening of arcs, auroral breakup, and appearance of NS forms) coincided with moments of local magnetic field dipolarization and an increase in the amplitude Pi2 of pulsations of the Bz component of the magnetic field on the satellite. Approximately 30–50 s before these moments, the magnetosphere was characterized by an increased rate of plasma flow in the radial direction, which initiated the formation of plasma vortices. The auroral activation delays relative to the times when plasma vortices appear in the magnetosphere decreased with decreasing latitude of the satellite projection. The plasma vortices in the magnetosphere are assumed to be responsible for the observed auroral vortex structures and the manifestation of the hybrid vortex instability (or shear flow ballooning instability) that develops in the equatorial magnetospheric plane in the presence of a shear plasma flow in the region of strong pressure gradients in the Earthward direction. 相似文献
12.
This paper presents the doses levels expected in orbits in chart form, covering the range 300-800 km of altitude and 0-90 degrees of inclination behind shieldings similar to the Hermes spacecraft and the EVA spacesuit matter distributions. These charts allow users to rapidly find the radiobiological dose received in the most critical organs of the human body either in normal situations or during a large solar event. Outside the magnetosphere, during interplanetary or lunar missions, when the dose received during crossing of the radiation belts become negligible, the dose is due to galactic cosmic rays (GCR) and solar flares. The correct radiobiological assessment of the components of this radiation field becomes a major problem. On the Moon a permanent ground-based station can be shielded by lunar materials against meteoroids and radiations. The radiobiological hazard, essentially linked to the solar flare risk during the transfer phase and the extra-station activities, may be solved by mission planning. For interplanetary flights the problem comes from both increased risk of solar events and from the continuous exposure to GCR. These energetic particles cannot be easily stopped by shieldings; cost considerations imply that more effective materials must be used. Impact on the vehicle design and the mission planning is important. 相似文献
13.
14.
Fluxes and differential spectra of 0.04–2.0 MeV electrons at low altitudes in the Earth's magnetosphere are considered in comparison with the model spectra AE-8 MAX and AE-8 MIN. Possible causes of the discrepancy between the observational and model spectra are discussed. The coefficients of radial diffusion at various L-shells are estimated for the maximum of solar activity (using the Interkosmos-19 data) and for the minimum of solar activity (using the Kosmos-1686 data) and are derived from the model AE-8. A quantitative evaluation of the electron yield from radial diffusion at low L shells is derived. Ionization losses, Coulomb angle scattering, and resonant wave–particle interaction are considered as the loss mechanisms. A calculation of these losses at the low L-shells is given. The electron distribution at low L-shells is best fitted by a combination of dissipative terms from different models: Coulomb scattering dominates at the lower L-shells (L = 1.2–1.4) and the resonant wave–particle interaction controls the radiation belt maximum and the gap (L = 1.4–2.0). 相似文献
15.
16.
S. V. Apatenkov T. M. Sugak V. A. Sergeev M. A. Shukhtina R. Nakamura W. Baumjohann P. Daly 《Cosmic Research》2009,47(1):22-28
Injections of energetic electrons with a dispersion over energies were observed during the February 23, 2004 (at about 03:20 UT) substorm onboard the Cluster satellites in the vicinity of perigee near the midnight meridian. The delays in the particle observation caused by the energy dependence of the magnetic drift velocities made it possible to determine the position and time of the beginning of the drift, tracing the trajectories of the leading center of particles back in time in the magnetospheric model. The comparisons of the measurements of four satellites allowed us to determine the radial propagation of the injection front with a velocity of 100–150 km/s at a distance of 7–9 R E. The comparison with a few previous measurements shows a substantial slowing down of injections as they approached the Earth, and this confirms the prospects of this method for more detailed study of propagation of plasma injection into the inner magnetosphere. 相似文献
17.
中能电子测量对空间辐射环境的理论研究和空间航天器的防护设计具有重要意义。北京大学研制的中能电子成像谱仪(BD-IES)利用小孔成像技术实现多方向中能电子的能谱测量。地面标定试验结果表明,BD-IES具有良好的能量线性度和较小的系统噪声,能够有效实现对中能电子的能谱测量。该仪器已成功应用在我国导航卫星上。最新测量结果表明BD-IES对中能电子的测量是成功的,其结果对于研究如亚暴注入、波-粒子相互作用等空间物理热点问题具有重要意义。BD-IES未来将被应用到"风云"等空间环境探测平台上。 相似文献
18.
We present the results of a cross-correlation analysis made on the basis of Spearman’s rank correlation method. The quantities
to correlate are daily values of the fluence of energetic electrons at a geosynchronous orbit, intensities of ground and interplanetary
ultra-low-frequency (ULF) oscillations in the Pc5 range, and parameters of the solar wind. The period under analysis is the
23rd cycle of solar activity, 1996–2006. Daily (from 6 h to 18 h of LT) magnetic data at two diametrically opposite observatories
of the Intermagnet network are taken as ground-based measurements. The fluxes of electrons with energies higher than 2 MeV
were measured by the geosynchronous GOES satellites. The data of magnetometers and plasma instruments installed on ACE and WIND spacecraft were used for analysis of the solar wind parameters and of the oscillations of the interplanetary magnetic field
(IMF). Some results elucidating the role played by interplanetary ULF waves in the processes of generation of magneospheric
oscillations and acceleration of energetic electrons are obtained. Among them are (i) high and stable correlation of ground
ULF oscillations with waves in the solar wind; (ii) closer link of mean daily amplitudes of both interplanetary and ground
oscillations with ‘tomorrow’ values of the solar wind velocity than with current values; and (iii) correlation of the intensity
of ULF waves in the solar wind, normalized to the IMF magnitude, with fluxes of relativistic electrons in the magnetosphere. 相似文献
19.
Cosmic Research - This paper presents the results of studies of the features of the injection of energetic electrons from the Earth’s radiation belt into the midlatitude ionosphere when the... 相似文献
20.
以木星探测任务为背景,针对木星辐射带粒子能量高、通量大的强辐射特点,基于器件总剂量辐照试验数据、木星辐射带模型、太阳质子通量模型,将器件失效点剂量不确定性与辐射环境不确定性应用到总剂量设计中,可定量评估特定任务一定屏蔽下的器件失效概率、辐射设计余量(RDM)的置信度及影响因素,可实现木星任务中器件指标、屏蔽厚度和失效概率之间的权衡和优化。首先,根据商业器件TL084辐照试验数据,发现其失效概率分布符合威布尔分布。对于10个木星半径的赤道面轨道,辐射带质子通量比太阳质子大3个数量级,随着屏蔽厚度的增加和任务期的减小,TL084器件所受剂量和失效概率减小。当屏蔽厚度为 10 mm 铝时,器件平均寿命小于2星期。另外,定义并考察了器件的失效速率,失效速率随屏蔽厚度的减小和在轨时间的增加而增加。对于传统的RDM为2的设计方法,1 mm铝屏蔽下对应的置信度为89%。 相似文献