Monitoring of solar proton events at altitudes up to 1000 km: Data from the Russian space experiments. Solar proton effects in the Earth’s ozonosphere

The paper illustrates the opportunities provided by the use of data from Russian satellite experiments (CORONAS and Universitetsky-Tatiana of Meteor series) on the measurement of fluxes and spectra of solar cosmic rays at altitudes of 370–1000 km for simulation of the ozonosphere state. The results of photochemical simulation and observational data analysis showing the influence of solar protons on polar ozonosphere and lower ionosphere in periods of solar proton events (SPE) on November 4, 2001, October 28, 2003, and January 16, 2005 are presented. It is shown that the solar proton action causes ozone depletion in the mesosphere above the polar regions. The strongest depletion (up to 70%) was caused by the SPE that occurred on October 28, 2003.     

不同高度和不同地磁扰动期间热层大气密度模式值与探测值的显著差异

热层大气密度是空间大气环境的重要参数,经过多年的研究已开发了多种大气模式,但其误差普遍较大,尤其在磁暴期间偏差值甚至超过100%.本文利用中国星载大气密度探测器和CHAMP卫星加速度计在轨获得的连续探测数据,针对近10年(2003—2014)中多次强磁暴事件和多次中等强度扰动事件,即2003年11月、2004年7月和2005年8~9月多次强磁暴事件(Kp值均达到9),2006年4月、2012年4月的两次中等强度磁暴事件(Kp值分别达到7和6),分析和比对不同强度磁扰事件期间不同高度全球大气密度就位探测值与模式值(NRLMSISE00)之间的差别.在2005年8月24日强磁扰事件中,560 km高度中国卫星就位探测值上涨幅度约2~3倍,扰动区中的增变比高达5.7倍,375 km高度CHAMP卫星就位探测值上涨幅度约0.8倍,扰动区中增变比达4.0倍,期间大气密度模式值不仅没有出现明显的涨落,更没有出现强烈的区域扰动;在2003年11月和2004年7月的强磁扰事件中,CHAMP卫星就位探测值均有显著涨变和强烈扰动变化,而模式值无明显扰动变化;在中等强度磁扰事件中,高度560 km附近就位探测值在北、南半球高纬地区显著上涨,远高于模式值,高度350 km附近就位探测值在地球阴影区域显著上涨,上涨幅度也大于模式值.分析结果表明现有大气模式对地磁扰动(尤其是强磁暴事件)期间全球热层大气密度的响应并不明显,需要进一步改善.     

Unusual sudden ionospheric disturbance from solar flare of 4 November 2003

An interpretation of the nature of the sudden ionospheric disturbance in terms of response to X-ray flux enhancement in the band 1–20 Å has been made by many authors. Last decades investigations revealed presence of important qualitative distinctions in spatially temporal pattern of geomagnetic response to solar flares featuring harder radiation spectra (with quanta energies above 100 keV). These distinctions can not be adequately described by classical theory implying ionization growing on E and D ionosperic layers and intensification of Sq-current system. In this respect, solar flare on 4 November 2003 characterizing by existence of two separate (time lag ~45 min) spectral maximums in X-rays range (average quantum energy <100 keV) and in γ-rays range (average quantum energy >100 keV), represents convenient proving ground for study of specifics the geomagnetic response to bursts marked by different hardness. In current article, we show that this flare has a number of unusual features including specific variation of accompanying current system and magnetospheric manifestation that is observed in trapped radiation fluxes and magnetic field on geosynchronous orbit. Possible physical mechanism leading to intensification of magnetospheric–ionospheric current system is discussed.     

Responses of geostationary orbit energetic electron fluxes to chorus waves under different geomagnetic conditions

We investigate the flux evolution of geostationary orbit energetic electrons during a strong storm on 24 August 2005(event A,the storm index Dst<200 nT,the average substorm index AE=436 nT)and a weak storm on 28 October 2006(event B,Dst>50 nT,average AE=320 nT).Data collected by LANL and GOES-12 satellites show that energetic electron fluxes increase by a factor of 10 during the recovery phase compared to the prestorm level for both events A and B.As the substorm continued,the Cluster C4 satellite observed strong whistler-mode chorus waves(with spectral density approaching 10 5nT2/Hz).The wave amplitude correlates with the substorm AE index,but is less correlated with the storm Dst index.Using a Gaussian distribution fitting method,we solve the Fokker-Planck diffusion equation governing the wave-particle interaction.Numerical results demonstrate that chorus waves efficiently accelerate~1 MeV energetic electrons,particularly at high pitch angles.The calculated acceleration time scale and amplitude are comparable to observations.Our results provide new observational support for chorus-driven acceleration of radiation belt energetic electrons.     

Flare Plasma Diagnostics from X-Ray and Ultraviolet Observations

We compare the measured values of emission measure EM and temperature T of coronal flare plasma following the GOES, RHESSI, and SDO/AIA satellite observations for the events of July 4, 5, and 7, 2012, in the NOAA 11515 active region. We show that the values of EM and T can vary widely (up to one order of magnitude for EM) depending on the technical features of instruments and processing technique. The maximum difference has been found to be between RHESSI and SDO/AIA measurements for temperature and between GOES and SDO/AIA measurements for EM. We discuss the pros and cons of the approaches used and the practical effects of the resulting numerical estimates for EM and T.

     

Certain features of UHF propagation during solar proton events

Results of the experimental reception of the UHF signal from geostationary satellite, visible at a low elevation angle from the receiving point, have been considered. It has been noted that the fluctuation intensity considerably increases during powerful solar proton events. The observed effect can be caused by interference between direct and secondary rays related to tropospheric irregularities. The hypothesis explaining obtained results based on the optical model of solar-tropospheric coupling is proposed.     

Spatial features of current systems of SFE-flares accompanied by gamma radiation

Based on statistical data and a detailed analysis of geomagnetic response to the hard electromagnetic radiation of the X17 solar flare of September 7, 2005, we considered spatial features of current systems producing the geomagnetic solar flare effect (SFE). During flares accompanied by intensive X-rays and gamma rays, SFEs are shown to be observed globally, including the night hemisphere and high latitudes. Cause-effect relations of phenomena under consideration are discussed.     

Modeling of Physical Processes by Analysis of Hard X-Ray and Microwave Radiations in the Solar Flare of November 10, 2002

For electron acceleration during solar flares, it is very important to determine the pitch-angle and energy dependences of the electron distribution function. At present, this cannot be done directly from observations. Therefore, it is necessary to perform a numerical simulation of the propagation of accelerated electrons in the magnetic field of the flare loop (loops) and calculate the X-ray and radio emissions. For the solar flare of November 10, 2002, we have obtained qualitative and quantitative agreements of modeled X-ray and radio maps with the RHESSI satellite and Nobeyama Radioheliograph data. We have determined the flare model parameters that agree with observations. The pitch-angle anisotropy of electrons determined by highly directional functions of the S(α) = cos⁸(α) type, the energy spectrum consist of two electron populations, the low-energy part of the spectrum up to an energy of break of 350 keV is characterized by a power law with the exponent δ₁ = 2.7–2.9, and the energy spectrum is more rigid above 420 keV (δ₂ = 2–2.3).     

Two-stage acceleration of solar cosmic rays

On the basis of data from the Radio Solar Telescope Network (RSTN), as well as the Geostationary Operational Environmental Satellite (GOES) and the WIND spacecraft, for the period from 1989 to 2006 covering 107 flare events, we investigated the relationship between the intensity of solar cosmic rays and parameters of continuum radio bursts (25?C15400 MHz), as well as type II radio bursts in the meter and decahectometer wavelength ranges. Proton fluxes with energies E _p > 1?100 MeV were calculated with regard to a reduced heliolongitude. The maximum correlation between solar cosmic rays and solar parameters of microwave bursts was 0.80. Its value was no more than 0.40 for the drift rate of type II bursts and 0.70 for the compression rate of coronal shock waves. Based on linear regression equations, we estimated the contribution of coronal shock waves to the acceleration of protons. We found that major acceleration processes occur in the area of burst energy release and complimentary processes occur at the fronts of coronal shock waves. The contribution of the latter to the acceleration process increases significantly with proton energy.     

Dynamics of radiation belt relativistic electrons in November 2004–January 2005

The radiation belt dynamics during the extreme solar events in November 2004 and January 2005 is studied based on the measurements of relativistic electrons (with energies of 0.8–8 MeV) on the Express-A2 geostationary satellite and Meteor-3M polar satellite. New radiation belts of relativistic electrons in the space (L ～ 3) between the stationary outer and inner belts were formed as a result of either superstorm (|Dst|_max = 373 and 289 nT). The position of the maximums of these belts (L _max = 2.9 and 3.1) coincides with the known dependence of L _max on the magnetic storm Dst variation amplitude: |Dst|_max = 2.75 × 10⁴/L _max ⁴ . In November–December the new belt very slowly (ΔL ～ 0.1 per month) shifted toward the Earth. During the series of moderate (～100 nT) magnetic storms that developed as a result of the extreme solar events in January 2005, the belt in the space shifted toward deeper L shells (L ～ 2.5). The moderate January storms produced new belts with L _max ≥ 4.     

Powerful nonstationary processes on the sun: Spatio-temporal structure and efficient particle acceleration

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.     

Superfine time structure and polarization of hard X-ray emission during solar flares: Simulation of isolated pulses

A superfine time structure has been detected recently via hard X-ray satellite observations during solar flares. Some pulses are hundreds of milliseconds in length. Time series are sharply nonstationary sequences of overlapping pulses. We interpreted a similar time structure in a model of the nonstationary kinetics of accelerated electron beams. In this work, we present calculation results of the degree of polarization of the hard X rays of solar flares with millisecond pulses. The dependence of the polarization degree on the plasma concentration, radiation energy, and the observation angle has been derived from calculations with the thick-target nonstationary kinetics model for rectangular and triangular individual pulses of accelerated electrons in the region of injection with the angular dependence cos²ⁿ θ. It is shown that the degree of polarization does not exceed 78% and decreases down to 50–65% 20 s after the beginning of the injection.     

2003年11月份日全食期间“创新一号”卫星母线电压异常的诱因分析

对2003年11月份发生在南极附近地区的日食事件进行了扼要介绍；利用STK软件，对日食事件进行了仿真计算，分析了造成11月23日日全食发生期间，CX-1卫星的母线电压异常的诱因.基于CX-1的最新轨道数据，利用STK软件，仿真了2004年CX-1卫星面临的日食事件，并给出了详细的时间表.     

Powerful solar radio bursts as a global and free tool for testing satellite broadband radio systems,including GPS–GLONASS–GALILEO

We investigated failures in the global positioning system (GPS) performance produced by solar radio bursts with unprecedented radio flux density during the X6.5 and X3.4 solar flares on 6 and 13 December 2006, respectively. The effect of these events on GPS was compared to that of the X17.2 solar flare of 28 October 2003. Significant experimental evidence was found that high-precision GPS positioning on the Earth's entire sunlit side was partially disrupted for more than 10–15 min on 6 and 13 December 2006. The high level of phase slips and count omissions resulted from the wideband solar radio noise emission. Our results provide serious grounds for revising the role of space weather factors in the functioning of modern satellite systems and for considering these factors more carefully in practice. Similar failures in the operation of satellite navigation systems (GPS, GLONASS, and GALILEO) can be fatal for operating safety systems as a whole and lead to great financial losses. Another important conclusion of our investigation concerns the continuous calibrated monitoring of the level of the solar radio emission flux. This monitoring involved a large number of solar radio spectrographs and allowed us to estimate the solar radio noise level in the range of the GPS–GLONASS–GALILEO frequencies.     

Observations of subterahertz radiation of solar flares with an RT-7.5 radiotelescope

We analyzed unique observations of two flare events at frequencies of 93 and 140 GHz. The observations were carried out with an RT-7.5 radiotelescope at the Bauman State Technical University (Moscow) using the method of continuous active region tracking with spatial resolutions of 2.5 (at a frequency of 93 GHz) and 1.5 arc-minutes (at 140 GHz). The light curves of the bursts were analyzed and compared with the time profiles of soft and hard X-ray emission obtained by the GOES and RHESSI spacecraft. The radio delete this word flux density spectra were plotted. It was found that the radiation flux at a frequency of 140 GHz exceeded the flux at 93 GHz. This constitutes a new independent confirmation of the presence of a subterahertz flare component, the appearance of which may be associated with the thermal radiation of the hot plasma at the base of flare loops.     

我国宇宙线空间物理学的进展

本文介绍了宇宙线空间物理学在我国的形成和主要研究内容,包括:(1)空间探测,有火箭探测、卫星探测;地面宇宙线台站观测;宇宙线的水下测量;(2)宇宙线空间物理学研究,有宇宙线的日地传输;宇宙线强度变化与CME事件;宇宙线的源物质与加速过程;宇宙线的地球物理效应.最后提到宇宙线与人体健康,特别是流行性感冒、大的太阳质子事件与地震现象、太阳宇宙线事件与天气和气候等的统计研究.     

Energetics of the magnetospheric superstorm on November 20, 2003

The magnetospheric storm on November 20, 2003 was one of two greatest events in 1957–2003. The D _st^* index reached −472 nT, the polar cap potential drop exceeded 200 kV, the polar cap boundary expanded up to Φ = 60°, the plasma layer density in the synchronous orbit reached 5 cm⁻³, and the inner edge of the plasma sheet penetrated up to L ∼ 1.5R _E. The sequence of disturbance modes including some previously unknown is described. The distribution of the total power input into the magnetosphere between the ionosphere (power Q _i) and the ring current (Q _DR), as well as the relative roles of the spontaneous substorms and the driven disturbances in the creation of the DR current, is analyzed. The values of the parameter α = Q _DR/Q _i are calculated with a step of 5 min. It is shown that intervals with α ≪ 1 and with maximums α ≫ 1 were observed in the events under consideration. These results contradict the dominant opinion that the energy input into the magnetosphere during disturbances is primarily dissipated in the ionosphere. The two types of α maximums are observed: one in the mode of a prevailing spontaneous substorm and the other in the mixed mode of the substorm and driven disturbance. It is concluded that both types of the maximums and corresponding enhancements of the DR current appeared due to the plasma turbulization processes in the substorm current wedge. The parameter α appears to slowly increase from α ≪ 1 to α > 1 with increasing activity level; this trend supports the driven model of creating the DR current due to an increase in the electric field of the solar wind.     

Regularities in solar high-energy particle fluxes: Experimental data and probabilistic model

The currently available experimental data, among which the series of particle flux measurements on satellites are of crucial importance, have revealed a number of regularities pertaining to solar cosmic rays (SCRs). Based on these regularities, we have developed a probabilistic model of particle fluxes. This model not only provides a basis for determining radiation conditions in space flights and space weather impacts but also allows such situations as the occurrence of extreme SCR events in the quiet-Sun period in 2005–2006 to be predicted.     

Geological constraints on the 2003–2005 ash emissions from the Nakadake crater lake,Aso Volcano,Japan

The active crater of Nakadake at Aso Volcano, southwestern Japan, has been occupied by a lake during its dormant periods. Multiple ash emissions were observed from the crater lake between July 2003 and August 2005. The largest events occurred on 10 July 2003 and 14 January 2004. On 10 July 2003, ash (41 tons) was dispersed throughout an area extending 14 km east-northeast of the vent, and on 14 January 2004 ash (32 tons) extended 8 km to the east-southeast. Thereafter, small ash emissions were frequent at the crater lake, in which the water level fell considerably from April to August 2005. During this period major ash emitting events, producing mostly white aggregated ash, occurred on June 10–12, June 21 (4.2 tons) and July 25 (1.2 tons). Ash emissions at the Nakadake crater in 2003–2005 were classified into three types: gentle release of white aggregated ash from fumaroles inside the crater lake (e.g. daytime of 14 April, 10–12 June and 25 July 2005); emission of black ash from an almost dried-up vent (21 June 2005); and short-time (ca. 20 s) small-explosion-triggered gas-and-ash emission through the crater lake (10 July 2003, 14 January 2004 and 14 April 20h41m 2005). All products from these ash emissions consisted of fine-grained (< 1 mm) glass shards, crystals and lithic fragments, and contained neither lapilli nor blocks. Although the glass shards show varying degrees of crystallization and alteration, clear glass shards, which appear fresh, are probably juvenile materials. These observations suggest that the 2003–2005 ash emissions from the crater lake of Nakadake Volcano are related to newly ascending magma.     

Dynamics of solar protons in the Earth’s magnetosphere during magnetic storms in November 2004–January 2005

The processes of penetration, trapping, and acceleration of solar protons in the Earth’s magneto-sphere during magnetic storms in November 2004 and January 2005 are studied based on the energetic particle measurements on the CORONAS-F and SERVIS-1 satellites. Acceleration of protons by 1–2 orders of magnitude was observed after trapping of solar protons with an energy of 1–15 MeV during the recovery phase of the magnetic storm of November 7–8, 2004. This acceleration was accompanied by an earthward shift of the particle flux maximum for several days, during which the series of magnetic storms continued. The process of relativistic electron acceleration proceeded simultaneously and according to a similar scenario including acceleration of protons. At the end of this period, the intensification was terminated by the process of precipitation, and a new proton belt split with the formation of two maximums at L ～ 2 and 3. In the January 2005 series of moderate storms, solar protons were trapped at L = 3.7 during the storm of January 17–18. However, during the magnetic storm of January 21, these particles fell in the zone of quasi-trapping, or precipitated into the atmosphere, or died in the magnetosheath. At the same time, the belts that were formed in November at L ～ 2 and 3 remained unchanged. Transformations of the proton (and electron) belts during strong magnetic storms change the intensity and structure of belts for a long time. Thus, the consequences of changes during the July 2004 storm did not disappear until November disturbances.