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提出了一个新的太阳宇宙线日 -地传输的数学模型 ,它包括日冕粒子分布源和行星际传播方程 .根据对太阳宇宙线耀斑黑子群特征和耀斑相的观测 ,提出了多极性黑子湮没的两阶段日冕传输过程和传输方程 ,得到了与观测特征一致的日冕粒子分布源 .日冕传输的第一阶段 ,和太阳耀斑脉冲相的时间相当 ,加速粒子通过扩散很快均匀地分布在耀斑区 ,形成所谓快传播区 .第二阶段 ,加速粒子向快传播区以外的日冕区扩散并向行星际空间逃逸 ,形成慢传播过程 .日冕传输模型的数值结果和日冕传输的观测特征符合 .太阳宇宙线的行星际传播采用三维正交均匀各向异性方程描述 .最后把模型的数值结果与 1 997年 9月 2 4日事件的SOHO（SolarandHeliosphericObservatory）观测资料作了比较 .能较好地符合 . 相似文献
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关于2003年10～11月日地关系重大事件研究综述 总被引：2，自引：2，他引：2
发生于2003年10～11月许许多多日地关系重大事件，西方称为万圣节日地事件或风暴(Halloween Events 或Halloween Storms),并予以特别关注.本文综述对这次日地重大事件的国际集会讨论和公开出版的文献，在太阳爆发方面包括：（1）太阳活动区与耀斑；（2）日冕物质抛射CMEs；（3）日冕激波；（4）太阳高能粒子SFPs；（5）活动区能量与面积、耀斑大小和CME速率.在日球层与地球物理效应方面，包括：（1）日球层响应；（2）大磁暴与宇宙线磁层效应；（3）热层与电离层效应；（4）白天极光、臭氧亏损；（5）中国学者工作.期望我国在此基础上积极开展工作和取得创新. 相似文献
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分七个方面扼要评述我国太阳大气和行星际动力学领域的近期成果：（1）耀斑的储能和释能；（2）日冕物质抛射；（3）行星际准定态结构；（4）行星际扰动和激波传播；（5）太阳风中的阿尔文起伏；（6）太阳宇宙线的传播；（7）磁流体（MHD）计算方法设计． 相似文献
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日冕物质抛射与太阳粒子事件 总被引：1，自引：0，他引：1
本文介绍了２０多年来对日冕物质抛射与太阳粒子事件的关系和太阳粒子事件的源等方面的研究成果和进展。大量的研究表明，太阳粒子事件源于日冕物质抛射并被日冕和行星际激波加速和控制。在无耀斑源的日冕和行星际激波加速和控制。只有极少数产生太阳粒子事件，并且这些事件中多数为低能粒子事件。这些相关日冕物质抛射的共同特征是：无相关的强Ｘ射线爆发，产生的行星际激波速度较快，无激波加速，无Ⅱ和Ⅳ米波爆发。几乎所有的产生 相似文献
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日冕物质抛射（ＣＭＥ） 是一个极为复杂的动力学过程本文基于开放场、闭合场的物理条件及射电爆发理论, 研究了ＣＭＥｓ 与相伴随的射电Ⅱ型、Ⅲ型、Ⅳ型爆发、软χ射线增强及太阳耀斑的关系给出了它们相伴随的条件： 当磁通量喷发, 能量释放时, 等离子体将被加速如果加速区在开放场, 可能会产生Ⅲ型爆发; 如果是闭合场, 被加速的高能质子和高能电子将被磁环捕获高能质子在磁环腿部呈损失锥分布, 当Ｅ≥ＥＴ 时会产生软χ射线增强随着磁环内的热压Ｐ和磁压Ｐｍ 的升高, 当β≥βＴ 时, 磁环将炸裂, 产生ＣＭＥｓ抛射出的高能相对论电子绕开放场线作螺旋飞行时, 会产生Ⅳ型爆发; 而亚相对论电子以零入射角沿开放磁场线逃逸时, 会产生Ⅲ型爆发高速飞行的等离子体产生激波时, 会产生Ⅱ型爆发当ＣＭＥｓ 源接近耀斑时, 会触发耀斑爆发 相似文献
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本文以行星际大尺度扇形磁场为基础,建立了研究太阳宇宙线在行星际传播较合理的扇形坐标系,并导出了太阳宇宙线在这种坐标系中的传播方程。同时研究了太阳宇宙线的一种扩散模型,扩散方程的解依赖于耀斑源在太阳上的磁径度,并得到了粒子强度随时间变化的特性,与观测结果比较,理论与观测资料符合较好。 相似文献
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风云二号系列卫星以自旋稳定方式工作于地球静止轨道,太阳X射线探测器是该系列卫星的重要有效载荷,监测太阳耀斑爆发过程,并对太阳质子事件等灾害性的空间天气事件进行预警.卫星自旋一周,该探测器完成一次全日面观测,记录太阳X射线的能谱与流量.2012年初,太阳活动进入第24周峰年,风云二号卫星太阳X射线探测器的在轨运行取得了良好的观测结果.相比于过去的太阳X射线探测器,风云二号F星的太阳X射线探测器应用了硅漂移探测(Silicon Drift Detector,SDD)技术,对GEO轨道海量的高能带电粒子采取了有效的屏蔽措施,可以对更"软"的X射线进行观测,能谱分辨率本领达到国际先进水平,对太阳耀斑的量化定级精度更高,在轨初步观测结果表明,精确的能谱探测能力可提高太阳质子事件预警能力,能道响应的时间特性比过去的探测数据更准确地反映了太阳耀斑的加热过程和带电粒子加速特性.本文介绍了风云二号F星太阳X射线探测器的设计及其发射前的标定试验结果,并且对发射后在轨运行获得的初步探测成果进行分析和讨论. 相似文献
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M.I. Sandanger F. Søraas M. Sørbø K. Aarsnes K. Oksavik D.S. Evans 《Journal of Atmospheric and Solar》2009,71(10-11):1126-1144
The losses of radiation belt electrons to the atmosphere due to wave–particle interactions with electromagnetic ion-cyclotron (EMIC) waves during corotating interaction region (CIR) storms compared to coronal mass ejections (CME) storms is investigated. Geomagnetic storms with extended ‘recovery’ phases due to large-amplitude Alfvén waves in the solar wind are associated with relativistic electron flux enhancements in the outer radiation belt. The corotating solar wind streams following a CIR in the solar wind contain large-amplitude Alfvén waves, but also some CME storms with high-speed solar wind can have large-amplitude Alfvén waves and extended ‘recovery’ phases. During both CIR and CME storms the ring current protons are enhanced. In the anisotropic proton zone the protons are unstable for EMIC wave growth. Atmospheric losses of relativistic electrons due to weak to moderate pitch angle scattering by EMIC waves is observed inside the whole anisotropic proton zone. During storms with extended ‘recovery’ phases we observe higher atmospheric loss of relativistic electrons than in storms with fast recovery phases. As the EMIC waves exist in storms with both extended and short recovery phases, the increased loss of relativistic electrons reflects the enhanced source of relativistic electrons in the radiation belt during extended recovery phase storms. The region with the most unstable protons and intense EMIC wave generation, seen as a narrow spike in the proton precipitation, is spatially coincident with the largest loss of relativistic electrons. This region can be observed at all MLTs and is closely connected with the spatial shape of the plasmapause as revealed by simultaneous observations by the IMAGE and the NOAA spacecraft. The observations in and near the atmospheric loss cone show that the CIR and CME storms with extended ‘recovery’ phases produce high atmospheric losses of relativistic electrons, as these storms accelerate electrons to relativistic energies. The CME storm with short recovery phase gives low losses of relativistic electrons due to a reduced level of relativistic electrons in the radiation belt. 相似文献
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Qualitative estimates of the relative iron and oxygen ions (Fe/O) in flows of solar cosmic rays from impulsive and long-duration solar flares are obtained for different ion energy ranges. The Fe/O value serves as a measuring unit for the known FIP effect in the solar atmosphere. It is shown that the FIP effect is most evident (maximum Fe/O values) in impulsive events for ions at energies <2 MeV/n. In long-duration events, the Fe/O value gradually decreases in parallel with ion energy and its maximum values are observable in the area of relatively low energies. The comparison of some flare models provided grounds for a qualitative explanation of the Fe/O behavior in response to changes in ion energies for both classes of solar cosmic ray (SCR) events. 相似文献
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本文利用相对論带电粒子的两个寝渐不变量,討論了磁暴主相期間外輻射带中心結构的变化。作者认为磁暴主相是由“磁暴带”环电流所产生。“磁暴带”假設位于外輻射带中心之外,它是太阳等离子体穿入磁层后形成的。本文对初始能量W=20Kev和W=1Mev的电子分別进行了計算。 結果表明,在磁暴主相期間电子向外漂移,其赤道投擲角減小,但镜点离地面距离增高。因此,主相时所观測到的极光,并不是由于地磁場的平緩下降使小投擲角电子注入大气层而形成的。此外,計数率降低的主要原因是由于力管截面膨胀造成的粒子密度減小以及电子減速,而电子減速与投擲角有关,由此决定了电子通量沿磁力线分布的变化。以上結果与探险者6号（Explorer Ⅵ）的观測一致。 相似文献
15.
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
16.
The direction and polarization degree of hard X rays (HXRs) in solar flares are studied. The continuous injection of relativistic electrons, which is implemented in powerful flares, is considered. The stationary relativistic kinetic equation is studied by using the method of expansion in terms of the Legendre polynomial and by integrating the equations for the expansion coefficients. The HXR characteristics are calculated using the bremsstrahlung relativistic cross-section for different angular and energetic electron distributions in the acceleration region. A high linear polarization degree of HXRs (??35%) has been obtained for narrow (??cos6??) beams of electrons with a soft spectrum (??E ?6); the polarization degree decreases with increasing quanta energy, whereas the directivity of a high-energy emission increases. This effect is absent for a nonrelativistic approximation. The considered model is applied to one of the most powerful flares in cycle 23, registered on October 28, 2003. The measured polarization degree values at relativistic energies (0.2?C0.4 and 0.4?C1 MeV) agree with the results achieved in the considered model when the electron energy spectrum index (?? = 2.5), angular distribution part (??cos6??), and the spectrum cutoff energy (E max = 1.3 MeV) were specified. 相似文献
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The challenges of ‘standard’ model of solar flares motivated by new observations with the spacecrafts and ground-based telescopes are presented. The most important problems are in situ heating of photospheric and chromospheric loop footpoints up to the coronal temperatures without precipitating particle beams accelerated in the corona, and the sunquakes which are unlikely to be explained by the impact of highenergy particles producing hard X-ray emission. There is also the long-standing ‘number problem’ in the physics of solar flares. It is shown that modern observations favored an important role of the electric currents in the energy release processes in the low solar atmosphere. Particle acceleration mechanism in the electric fields driven by the magnetic Rayleigh-Taylor instability in the chromosphere is proposed. The electric current value I ≥ 1010 A, needed for the excitation of super-Dreicer electric fields in the chromosphere is determined. It is shown that both Joule dissipation of the electric currents and the particles accelerated in the chromosphere can be responsible for in situ heating of the low solar atmosphere. Alternative model of the solar flare based on the analogy between the flaring loop and an equivalent electric circuit which is good tool for the electric current diagnostics is presented. Interaction of a current-carrying loop with the partially-ionized plasma of prominence in the context of particle acceleration is considered. The role of plasma radiation mechanism in the sub-THz emission from the chromosphere is discussed. 相似文献
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日地系统学中的太阳活动研究（Ⅱ）爆发型太阳活动—太阳耀斑 总被引：1，自引：0，他引：1
爆发型太阳活动是日地系统中重要的扰动源。本文介绍日地系统学中最剧烈的爆发型太阳活动－太阳耀斑的观测研究进展。综述了最近两个太阳周的地面与空间观测所得到的耀斑的物理图象和统计性质，简单讨论了空间观测设备的发展和面临的研究课题。 相似文献
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P. V. Vatagin Yu. E. Charikov A. V. Stepanov I. V. Kudryavtsev 《Geomagnetism and Aeronomy》2012,52(8):1015-1020
Unique measurements by a solar submillimeter radio telescope (SST) have been carried out in the sub-THz radiation at 212 and 405 THz over the past decade. The spectrum of RF radiation in this region increased with frequency for the three flares of November 2 and 4, 2003, and December 6, 2006, and the flux value reached 5 × 103?2 × 104 sfu at 405 GHz (Kaufman et al., 2009). In this work, we consider a set of nonlinear equations for an accelerated electrons beam and the Langmuir wave energy density. The distribution functions of the accelerated electron beam and wave energy density are calculated taking into account Coulomb collisions, electron scattering by waves, and wave scattering by plasma ions. In addition, the source of accelerated particles and the heat level of the Langmuir turbulence are specified. The beam and plasma parameters are chosen based on the aims of a problem. The plasma concentration varies from n = 1013 to 1015 cm?3, the electron plasma frequency f p = (3 × 1010?3 × 1011) Hz in this case. The ratio of plasma and beam concentrations, sufficient to explain the value of the radio flux at a frequency of 300 GHz, is n b/n = 10?3. The Langmuir turbulence is excited due to the instability of the accelerated electron beam with an initial distribution function of the ??bump-in-tail?? type. Then, the parameters of radiowaves are calculated in the sub-THz range under the assumption of coalescence of two plasma waves. The calculation results show that a sub-THz radio flux can be obtained under the condition of injection of accelerated electrons. The fine time structure of radio flux observed is easily simulated based on this statement by the pulsed time structure of electron beams and their dynamics in overdense plasma. X-ray and gamma radiation was recorded during the events under study. Hard X-ray radiation is bremsstrahlung radiation from accelerated electron beams. 相似文献
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Based on observations of electromagnetic radiation, a concept of thermal solar flares has been proposed. The absence of hard X-ray emission implies no accelerated electrons. This fact is the basis of the proposed concept of thermal flares. Since the acceleration rate should not exceed the electron energy loss rate, plasma density in the acceleration range must be at least 1011 cm?3. The temperature of plasma emitting in the soft X-ray range is of the order of 107 K. In the simplified problem of heated plasma hydrodynamics, we calculated the temperature profiles and their changes over time and by coordinate. The emission measure values determined from observations of the soft X-ray emission of flares is of the order of 1045 cm?3. The geometry of the source is an axial symmetric straight cylinder with a section of 1016 cm2 and an axial coordinate determined by the depth of plasma heating. Time profiles of soft X-ray emission were calculated for different sources of plasma heating, which were simulated using the Gaussian distribution law with respect to the coordinate and time. We have considered two modes of plasma heating: single (in time) and multipulse modes with different pulse intervals. The dynamics of plasma heating and cooling was shown to control the experimentally observed time profiles of soft X-ray emission. A comparison of numerical results with observational data allows us to confirm the implications of the proposed concept of thermal flares and, in addition, to perform diagnostics of plasma parameters in the emission source. 相似文献