Study of dynamics of global disturbances of the Earth’s magnetosphere using muon detectors

Amethod is developed, whichmakes it possible to predict in advance disturbances in the Earth’s magnetosphere, caused by solar flares or changes in the heliospheric magnetic field, since the cosmic particle flux reaches the Earth much earlier than coronal plasma bursts. To scan the celestial hemisphere, wide-aperture muon detectors are used. A unique system of muon hodoscopes was developed at the NEVOD Science and Education Center (MEPhI, Moscow). The data of the URAGAN muon hodoscope on two-dimensional dynamics of the muon flux during the Forbush effect of November 14, 2006 are analyzed. Changes in the muon flux intensity, measured at various directions with an interval of 30 min are shown. The results obtained demonstrate the muon flux sensitivity to solar plasma cloud motion, which offers prospects to use muon detectors to probe interplanetary space at long distances from the Earth and to predict geomagnetic disturbances.     

Phase fluctuations model for EM wave propagation through solar scintillation at superior solar conjunction

Traveling solar wind disturbances have a significant influence on radio wave characteristics during the superior solar conjunction communication. This paper considers the impact of solar scintillation on phase fluctuations of electromagnetic (EM) wave propagation during the superior solar conjunction. Based on the Geometric Optics approximation, the close-form approximation model for phase fluctuations is developed. Both effects of anisotropic temporal variations function of plasma irregularities and their power spectrum are presented and analyzed numerically. It is found that phase fluctuations rapidly decrease with increasing Sun–Earth–Probe angle and decrease with increasing frequency at the rate of 1/f². Moreover, the role of various features of the solar wind irregularities and their influence on the EM wave characteristic parameters is studied and discussed. Finally, we study the phase fluctuations of typical cases in order to better understand the impact of phase fluctuations in future deep space communication scenarios during solar conjunction periods.     

Effect of solar eclipses on neutron flux variations at the Earth’s surface

The results of the investigation of the neutron flux variations at the Tien Shan high-altitude scientific station during solar eclipses on September 23, 1987; August 11, 1999; and March 29, 2006 are reported. It is established that, during these periods, the dynamics of neutron intensity variations in the frequency range 10^?5–10^?3 Hz is due to geophysical sources of disturbances. An increase in the thermal neutron flux from the Earth’s Crust is observed.     

Propagation and Damping of Two-Fluid Magnetohydrodynamic Waves in Stratified Solar Atmosphere

An extreme ultra-violet(EUV) wave is characterized as a bright pulse that has emanated from the solar eruption source and can propagate globally in the solar corona. According to one leading theory, the EUV wave is a fast magnetoacoustic wave, as the coronal counterpart of the Moreton wave in the chromosphere. However, previous observations have shown that the EUV wave differs significantly from the Moreton wave in both velocity and lifetime. To reconcile these differences, here we analyze the wave characteristics of a two-fluid MHD model in the stratified solar atmosphere with a height-dependent ionization rate. It is found that the collision between neutral and ionized fluids is able to attenuate the wave amplitude, while causing a slight change in its propagation velocity. Because the chromosphere has the lower ionization rate and the stronger magnetic fields than the corona,the velocity of the Moreton wave is much higher than that of the EUV wave. In contrast to the Moreton waves damped strongly by the collision between neutral and ionized fluids, the EUV wave in the fully ionized corona is able to propagate globally on a time scale of several hours. Our results support the previous theory that fast magnetoacoustic waves account for both EUV and Moreteon waves in the different layers of the solar atmosphere.     

Faint Young Sun,Planetary Paleoclimates and Varying Fundamental Constants

The effect of a cosmic time variation of the gravitational constant on the solar luminosity evolution is studied. It is demonstrated that a varying gravitational constant can substantially affect the solar flux at the planetary orbits on geological time scales. Mean surface temperatures well above the freezing point of water can be achieved in this way throughout the Archean and Hadean, without invoking an increased greenhouse effect or a lower albedo. Instead of a monotonous decline of the solar flux in look-back time, due to a dim early Sun, we infer a flux minimum during the Early Proterozoic and Late Archean. In this epoch, the solar flux is capable of generating mean surface temperatures between 7^∘C and 12^∘C, as compared to the present 15^∘C. The flux then steadily increases, culminating in temperatures between 12^∘C and 19^∘C some 4.5 Gry ago, depending on the parameters chosen for the ‘standard’ Sun. This explains the absence of polar caps, and even warm oceans in the Archean and Hadean are possible at these temperatures. No change of the present 33 K greenhouse effect is required. As for Mars, we show that the solar flux at the Martian orbit before 3.8 Gyr was at least 90% of the present-day flux, so that mean surface temperatures above the freezing point could have been generated by CO₂ greenhouse warming. The time variation of the gravitational constant is such that the moderate dimensionless ratio ħ² H₀/(k₀ cm_π³) stays constant in cosmic time. There are stringent bounds on the logarithmic time derivative of the gravitational constant from lunar laser ranging and helioseismology, which indicate that the first-order derivative at the present epoch is too small to noticeably affect the solar luminosity evolution within the age of the Earth. However, higher-order derivatives have to be taken into account, as they do affect the solar flux in geologic look-back time. We consider the impact of a varying gravitational constant on the redshift scaling of the linear size of radio galaxies. The observed scaling exponent also enters the solar luminosity evolution. The age of the universe has a substantial imprint on planetary paleoclimates.     

Propagation of solar cosmic rays in loop-like interplanetary magnetic field structures

Features of propagation of relativistic solar cosmic rays in magnetic clouds have been considered on the basis of model calculations. Magnetic clouds have a structure of magnetic flux ropes and are extended from the Sun to the Earth via coronal mass ejections. Features of propagation of particles of different energies in a magnetic cloud are discussed. The propagation of high-energy solar protons in the loop-like structure of the interplanetary magnetic field in the event of October 28, 2003 is analyzed.     

Disturbances of the upper atmosphere and ionosphere caused by acoustic-gravity wave sources in the lower atmosphere

The results of observations of acoustic-gravity waves in the troposphere and the ionosphere at middle latitudes during periods of passage of the solar terminator are presented. Tropospheric observations were performed using a lidar. The frequency characteristics of variations of the tropospheric parameters are determined based on observations of the intensity of the scattered lidar signal. The characteristics of variations of the total electron content (TEC) in the atmosphere are determined from data collected by GPS navigation satellites. An analysis of the observational data showed that the spectrum of variations of the atmospheric and ionospheric parameters is indicative of acoustic-gravity waves (AGW) propagating from the lower atmosphere. Modeling studies of the vertical propagation of AGW from the Earth’s surface showed that such waves quickly (within ~15 min) reach altitudes of the upper atmosphere (~300 km). The refraction and dissipation of waves in the upper atmosphere produces perturbations of the background state of the atmosphere and gives rise to the waveguide propagation of infrasonic wave components. The observed manifestations of TEC disturbances caused by AGW propagating from the lower atmosphere can be explained by the diurnal variation of the altitude of the ionosphere and the waveguide propagation of infrasonic waves.     

Role of equilibrium plasma flow on damping of slow MHD waves

In the solar corona waves and oscillatory activities are observed with modern imaging and spectral instruments. These oscillations are interpreted as slow magneto-acoustic waves excited impulsively in coronal loops. This study explores the effect of steady plasma flow on the dissipation of slow magneto-acoustic waves in the solar coronal loops permeated by uniform magnetic field. We have investigated the damping of slow waves in the coronal plasma taking into account viscosity and thermal conductivity as dissipative processes. On solving the dispersion relation it is found that the presence of plasma flow influences the characteristics of wave propagation and dissipation. We have shown that the time damping of slow waves exhibits varying behavior depending upon the physical parameters of the loop. The wave energy flux associated with slow magnetoacoustic waves turns out to be of the order of 10⁶ erg cm⁻² s⁻¹ which is high enough to replace the energy lost through optically thin coronal emission and the thermal conduction below to the transition region.     

Solar-neutrino variations: A manifestation of nonzero neutrino mass and magnetic moment, and mixing

Time variations of solar neutrino flux are investigated on the basis of available Homestake experimental data for more than two solar cycles (1970–1994). At first, we determine (with the weight-time function by taking into account ³⁷Ar decay), for each solar neutrino run n, the effective Earth’s heliolatitude L _eff(n), the effective Zurich sunspots number Z _eff(n), the effective latitude of sunspots distribution Λ_eff(n), and the effective surfaces of sunspots in different heliolatitude belts. Then, we consider the correlation of solar-electron-neutrino fluxes with these parameters for different periods of solar activity. It is found that correlation coefficients change sign in different periods of solar activity, so that for total period 1970–1994 the correlation coefficient is very small. The obtained information indicates that a neutrino should have nonzero mass and nonzero magnetic moment.     

Analysis of the anisotropy of the muon flux, according to data obtained by the URAGAN muon hodoscope during heliospheric disturbances

Features of studying heliospheric disturbances caused by changes in the parameters of the interplanetary magnetic field by the anisotropy of the muon flux of cosmic rays detected on the surface of the Earth by the URAGAN muon hodoscope are considered. The anisotropy of the muon flux in the period 2007–2011 is analyzed. The forecasting potential of our approaches to studying heliospheric disturbances using the penetrating component of cosmic rays is evaluated.     

可获得高分辨率谱线信息的新型太阳极紫外成像仪

极紫外光谱观测和诊断是研究太阳大气基本物理过程的最重要手段之一。但因为波长短,很多可见光仪器的设计方案不再适用,且极紫外观测只能在太空中开展。国际上现有卫星上的太阳极紫外成像仪和光谱仪都有各自的不足,比如极紫外成像仪不能获得高光谱分辨率的谱线信息;狭缝式光谱仪通过扫描可得到活动区域的信息,但扫描时间过长,对于研究剧烈变化的太阳活动有很大的局限性。这些不足制约了对日冕物质抛射(CME)和耀斑等太阳活动的高精度观测及对其机理的研究：无法看到CME在内日冕的加速过程,而且无法将可见光看到的CME现象同极紫外看到的日面源区直接联系;缺少观测目标的视向速度信息,难以识别CME的触发过程。采用多级衍射成像方式的一种新型太阳极紫外成像仪,除实现传统极紫外成像仪功能外,还可以在太阳活动变化过程中同步获得全日面各区域的光谱信息。新型成像仪可以得到高光谱分辨率数据,用于反演低日冕的等离子体视向速度,获得全日面的速度分布,与同时得到的高空间分辨率图像相结合,可以识别太阳活动现象对应的物质运动, 为空间科学研究提供数据;因为没有狭缝和运动部件,可以实现对大视场的太阳活动区域的高时间分辨率成像,有利于捕捉日面活动的快速变化。新型成像仪采用无狭缝光谱分光成像的设计理念,即同一时间把一定光谱带宽的信息记录到一个二维的图像上,此过程可以看成是从某一个角度将空间和光谱数据立方体投影到一个面上,然后再利用反演得到空间分辨图像和光谱信息。多级光谱成像的光学设计与传统光谱仪最大的不同是其不存在逐行扫描的狭缝,这使得其能够同时获得大视场内太阳的空间信息和光谱信息。因为极紫外波段的特殊性,以及本仪器面向卫星遥感应用,不可能像可见光波段或者医用CT机一样实现很多衍射级的同时成像。因此,新型极紫外成像仪光学系统由反射镜、色散光栅和五个探测器组成,入射的太阳极紫外辐射经过光栅色散后分别由五个级次的探测器接收,其中四个探测器分部接收±1和±2衍射级图像,另外一个接收0级图像。空间信息可以直接从0级图像得到,而光谱信息则需要根据五个级次成像的反演结果得出。介绍了光学系统的设计以及反演算法,并分析了反演算法的误差。光路基于变间距光栅设计,可实现空间分辨率1.8 arcsec·pixel-1, 光谱分辨率7.8×10-3 nm·pixel-1,同时减小了体积和重量,适合空间应用。     

The correcting role of unusual heliocentric atmospheric phenomena

Research has been done on solar-terrestrial correlations on the basis of the organism model for the Earth, which suggests that the Earth affects the Sun by means of a natural energy and information flow and as a result of man-made factors. Changes in the Earth pattern affect regular processes in the solar system and cause new formations in solar activity. Solar-terrestrial correlations represent an energy and information flux and provide regulation mechanisms for the biosphere and the climatic engine on an evolutionary basis in strict agreement with the evolution of the solar system.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 3, pp. 105–110, March, 1992.     

Relativistic SCRs during the events of solar cycle 19

Two major ground-level SCR events in solar cycle 19 are analyzed: the events of May 4 and November 12, 1960. The characteristics of relativistic solar protons (RSPs) have been obtained using the up-to-date method based on the data from the ground based network of neutron monitors. The event of May 4, 1960, occurred against a quiet background, and during the event of 12.11.1960 two shocks, caused by previous flares in the same active region, approached the Earth. The RSP dynamics, related to disturbances in the interplanetary medium, is studied. The solar proton spectra, obtained from the ground-based measurements, are compared to the direct balloon measurements performed at that time.     

Photometry of solar EUV radiation by space-based telescopes with normal incidence multilayer-coated optics

Photometric methods of image analysis in the extreme ultraviolet (EUV) wavelength range are widely used in solving current scientific problems of solar physics. Types of solar EUV telescopes, their main parameters, effects of space flight and observation conditions on accuracy of the photometric analysis are considered.     

Evaluation of the energy spectrum of solar protons according to the balloon measurement data and Monte Carlo simulation

The method for evaluating the energy spectra of solar protons at the boundary of the Earth’s atmosphere according to the data of balloon measurements carried out at the Lebedev Institute of Physics, Russian Academy of Sciences, and the results of Monte Carlo simulation of the processes of proton interaction in the Earth’s atmosphere has been developed. The balloon measurements during solar proton events make it possible to determine the absorption spectra of solar cosmic rays in the atmosphere. Comparison of the experimental data with the results of the simulation of propagation of solar protons (E _p = 10 MeV-10 GeV) in the atmosphere, based on GEANT-4, allows determination of the energy spectra of solar protons at the atmospheric boundary. The results of the determination of the energy spectra of solar protons in a number of solar proton events in the current (23th) solar activity cycle are reported.     

Time of arrival of the first relativistic solar protons to the Earth

The anticoincidence system of the spectrometer onboard the INTEGRAL spacecraft (ACS SPI) is sensitive to primary and secondary γ-rays with energies higher than 150 keV and effectively responds to the arrival of solar protons and electrons. When the flux of primary γ-rays is small, ACS SPI registers the arrival of solar protons much earlier than the network of neutron monitors (NMs). For example, on December 13, 2006, ACS SPI registered the arrival of solar protons approximately 10 min earlier than the CR intensity started increasing on the Earth according to the NM data. However, when the flux of solar γ-rays is sufficiently high, ACS SPI observes the arrival of solar protons simultaneously with NMs (the event of January 20, 2005) or later (October 28, 2003). Found times of arrival of relativistic solar protons to the Earth do not contradict proton acceleration during γ-ray flares.     

Measurements of neutron fluxes with energies from thermal to several MeV in near-Earth space: SINP results

Neutron measurement results obtained at SINP MSU since 1970 are presented. These measurements were made using techniques based on neutron moderation and subsequent detection in a Li6I(Eu) crystal or a He3 coronal counter. The measurements were mainly carried out in orbits with inclination of 52 degrees and altitudes of 200-450 km. The spatial and angular distributions of the measured neutron fluxes were studied. The albedo neutron flux was estimated according to the count rate difference for opposite detector orientations towards Earth and away from it. This flux is comparable to the local neutron flux outside the Brazil anomaly region, where local neutrons dominate. Neutron fluxes, generated by solar protons, were detected during a solar flare on June 6, 1991 for the first time. Their spectrum was estimated as a power law with alpha>2.     

The space environment monitor aboard FY-2 satellite

The space environment monitor (SEM) aboard FY-2 satellite consists of the high energy particle detector (HEPD) and the solar X-ray flux detector (SXFD). The SEM can provide real-time monitoring of flare and solar proton event for its operation at geostationary orbit and is also the first Chinese space system for monitoring and alerting solar proton event. During the 23rd solar maximum cycle, almost all the solar proton events that took place in this period are monitored and some of them are predicted successfully by analyzing the characteristics of X-ray flare monitored by the SEM. Some basic variation characteristics of particle at geostationary orbit are found such as day-night periodic variation of particle flux, the electron flux with energy >1.4 MeV in the scope from 10 to 200/cm2 s sr and the proton flux with energy >1.1 MeV in the scope from 600 to 8000/cm·s·sr during the time with no magnetic storm and solar eruption.     

Approximately 2400-Year Cycle in the Concentration of Cosmogenic Radionuclides: Sources of Variations

Cosmogenic isotopes, including ¹⁴C, ¹⁰Be, and ⁷Be, are produced in the Earth’s atmosphere under the effect of cosmic rays. The rate of their production is determined by several factors, such as the intensity of primary galactic cosmic rays, the level of solar activity, and the strength of the Earth’s magnetic field. Changes in the isotope concentrations and distributions receive contributions from mixing processes proceeding in the surrounding medium: the atmosphere, biosphere, and oceans. The isotopes ¹⁴C and ¹⁰Be are the most important for studying solar activity and climate. Investigation of isotope concentrations reveal that there are both long-term trends and cyclic components. As for ¹⁴C, the long-term component caused by the change in the magnetic dipole moment of the Earth with a characteristic time of about 10⁴ years is the most commonly known. It is well known that the concentrations of cosmogenic isotopes change cyclically with time. The ~2400-year cycle (Hallstatt cycle) and the ~210-year cycle (de Vries cycle) are the most famous. In the present article, we discuss the possible origin of the ~2400-year cycle.     

塔式吸热器中辐射传播过程的参数分析

采用自编程的蒙特卡罗光线追迹程序模拟了太阳辐射在吸热器中的传播过程,计算求得了吸热体内的热流密度分布情况。由随机光于的传播特性可知,不同的系统参数会对吸热体内辐射分布产生影响。根据太阳辐射在吸热器中的传播顺序,本文依次考察了入射光倾角、多孔介质的几何形状以及厚度、吸收系数与消光系数比值(μ_a/μ_t)以及孔隙率(ε)等因素对SiC泡沫金属吸热体内吸收辐射分布的影响。计算结果表明入射光倾角和吸热体的几何形状是影响吸热体内热流分布均匀性的主要因素,且随着μ_a/μ_t比值的降低和ε的增加,吸热体内热流密度极值迅速减小,同时厚度方向的热流密度梯度变缓。本文的研究结果可以为太阳能吸热器的结构设计和材料选择提供参考。