探测地球自然灾害的一种方法

通过探测地球整体的辐射温度变化,即在空间把地球作为一个辐射点源对待,同时又将地球分成几百个局部,视为一个面源,进行实时的比较;又分别对太阳和宇宙背景的辐射温度变化进行测量,来了解地球表面和地气的热温度状况和太阳对地球、对宇宙背景能量传输的情况。从而研究地球上大规模灾害性事件(包括火山的爆发、地震、大气环流、气候变异等…)在整个地球上所能反映的热温度效应。探测地球在宇宙空间非平衡热状况下(太阳温度6000K;地球温度300K;空间背景3K)的耗散结构,研究在这种状况下物理力学的一些自会聚和自组织现象(即地球上灾害性事件形成过程),形成一门非平衡宇宙热力学,并使之成为一门实验科学。文章着重介绍为此目的实施的探测方法和其应用前景。     

大气中子实时计算模式

为实时评估0~100km高度范围内的大气中子全球分布,对宇宙线在地磁场和大气中的传输过程进行了分析.利用蒙特卡罗方法工具包Geant4,预先计算不同能量的粒子在大气层中产生的次级粒子能谱分布,形成大气次级粒子数据库,并与相关模型进行对比,验证了该数据库的有效性和可靠性.以实测或预报的空间环境参数作为输入,计算同步轨道银河宇宙线和太阳质子事件能谱以及100km高度上的地磁垂直截止刚度,最终得到大气层顶上的粒子能谱.通过对大气次级粒子数据库的线性插值,实现1h分辨率的大气中子能谱和辐射剂量全球分布的实时计算.      

太空行走100问（十四）

太空行走风险(上) 80.航天员在太空行走中可能会遇到哪些风险? (1)太空环境因素方面的风险: ①宇宙辐射 在近地空间的宇宙辐射属于电离辐射,主要有三个来源:地球辐射带、银河宇宙线和太阳粒子事件.     

太阳光谱辐射强度变化对地球能量平衡的影响分析

目前太阳对地球能量平衡影响的研究大都是以太阳总辐射通量密度作为输入参数的. 本文以美国航空航天局（National Aeronautics and Space Administration,NASA）太阳辐射与气候实验项目的卫星实测数据为基础,对太阳上升相（2010年上半年）和下降相（2007年12月）期间太阳光谱变化对地球能量平衡的影响进行了研究. 结果表明,2010年上半年较强的太阳总辐射通量密度主要是由紫外及红外波段的能量增强引起的,其在200～400nm 和760～4000nm波段内的平均能量分别增加了0.11%和0.05%,而在 400～760nm可见光区的能量却呈减小趋势,平均减小量为0.05%. 通过对MLS2.2全球臭氧日数据进行再分析后发现,相对于2007年12月,2010年上半年平流层臭氧浓度也有所增加,其中在太阳紫外辐射呈现较大增强的2月和3月,其臭氧增量也相对较大,最大值分别出现在33km和40km处,值为0.6mL·m-3和0.62mL·m-3. 因此,可见光区能量减弱与平流层臭氧浓度增加的双重削弱作用致使虽然2010年上半年的太阳总辐射通量密度较大,但是到达对流层顶的太阳辐射却有所减小,最大减小量出现在3月,值为0.15W·m-2. 这一结果说明,太阳活动或总辐射通量密度的增强也有可能对地球对流层系统起到冷却作用.      

大气中宇宙射线绝对电离量的测量

宇宙射线是环境中天然辐射的主要组成部分,来自银河系的初级宇宙线,进入大气层以后,由于产生一系列的级联过程以及大气对宇宙线的吸收作用,使得宇宙射线粒子的组成、强度以及能谱沿大气层的高度不断变化,同时由于受到地磁场的强烈影响以及11年太阳活动周期的调制,使不同纬度上不同年份的这种高度分布亦不相同。     

宇宙辐射,是资源还是祸害?

不是所有的东西都能成为太空家园的资源.有些不仅不是资源反而是祸害,宇宙辐射就是其中一例。 太空中的宇宙辐射对人体危害最大的主要是银河宇宙线和太阳宇宙辐射。银河宇宙线的主要成分是高能质子和原子序为偶数的重离子。太阳粒子事件产生大量的高能粒子,其中主要是质子、重粒子和电子。对人体危害最大的是质子,其次是重粒子。     

近地环境的电状态

通过电过程的耦合是太阳对气象耦合影响的机制之一,本文扼要地综述了迄今为止人们对近地环境内电流和电场的观测结果以及在此基础上所建立的经验和理论模式;给出了在平均状况下和太阳活动下近地环境电性能的总概貌,重点在靠近地球表面的低层、中层大气区域;着重介绍了该区域内的大气电性能及其受太阳活动的调制.      

耀斑脉冲相离子电离的弛豫过程

观测表明:在耀斑前活动区上空的日冕中普遍存在低温的磁环结构, 其中一些这种磁环结构的温度在105K以下;同时, 耀斑脉冲相存在非常迅速的加热过程.本文在这些观测事实的基础上, 提出了一个太阳耀斑爆发时离子电离的模型, 并由这一模型研究了耀斑时离子电离的弛豫过程.在太阳宇宙线的源物质来自高色球层的条件下, 得到了与观测结果符合得较好的太阳耀斑能量离子的平均电荷及其电离态分布.      

太阳宇宙线源物质的高色球层模式和重离子丰度过量机制的探讨

本文利用太阳能量粒子事件中重离子平均丰度过量的资料,计算得到太阳能量粒子源物质的温度,提出了描述太阳宇宙线能量粒子源物质的新模式——高色球层模式;太阳耀斑观测确定,太阳宇宙线耀斑的加速区一般最可能出现在低日冕甚至高达几万公里的高度,从而,太阳宇宙线的源和加速区通常不位于同一区域;进而提出了描述太阳能量粒子事件中重离子丰度过量的可能机制——其源物质是通过太阳黑子的冻结型无力场从高色球层输送到活动区,形成耀斑前加速区内重离子丰度大和耀斑后宇宙线中重元素丰度的过量.      

基于钠激光雷达观测数据的中间层顶大气温度分布特性研究

作为中间层和热层的边界层,中间层顶存在多种能量交换方式,是大气能量耦合的重要区域。本文利用部署于中国科学院廊坊临近空间大气探测站的钠荧光多普勒激光雷达2013年的观测数据,研究了廊坊上空中间层顶区域大气温度的年度和季节分布特性,并分析了影响温度分布的多种因素。年平均温度廓线图显示,中间层顶位于约97.5 km高度处,温度约191.2 K。受放热化学反应的影响,年平均温度廓线91 km高度处出现了一个198 K的相对温度高点。中间层顶区域大气温度的季节分布受太阳辐射和大气动力学因素综合影响,夏季在大气动力学影响下,中间层顶高度较低,位于88 km高度处,温度也较低,约177 K;冬季太阳辐射起主导作用,中间层顶位于99 km高度处,温度为181 K。通过拟合月平均温度分析了中间层顶区域大气温度年变化和半年变化的振幅和相位特征。结果显示,中间层顶区域上部温度分布主要受太阳辐射的影响;在中间层顶区域下部,大气波动主导了温度分布。      

A Mechanism of Solar Variability Effect on Radiative Balance of the Earth Atmosphere

Possible mechanisms of solar-climatic connections, which may be of importance as over short and long time intervals, are discussed. The variations of energetic balance of Earth's climatic system for the last fifty years are estimated. It is ascertained that the disbalance between the flux of solar energy that comes to the Earth and radiates to space is of 0.1% for the last ten years. The suggested mechanism makes it possible to explain not only the observed variation of the enthalpy of the Earth's climatic system for the period 1910-1980, but also the climate anomalies during last thousand years: the climate optimum in 12 century, and"small glacial period" in 16-17 centuries.      

太阳发电机理论研究

太阳活动主要是由磁场产生的, 因此, 对太阳磁场性质和起源的研究具有重要意义. 太阳发电机理论主要研究的是太阳上观测到的与太阳活动相关的磁场起源、磁场特征、各种活动现象之间的相关性及其变化规律. 其是太阳物理学中有待解决的最基本、最重要的问题. 根据太阳黑子及太阳周期的相关观测, 介绍了构成发电机的基本要素, 具体描述了各种典型发电机模型, 并对其分别进行评述, 进而探讨了目前存在的问题及发展方向.      

第22与23周磁静日北京台银河宇宙线周日变化与半日变化特征

利用快速傅里叶变换及其计算功率谱的方法研究了第22和23周磁静日北京宇宙线台站记录的银河宇宙线强度的周日变化与半日变化，计算结果表明，在两个太阳活动周交替时，银河宇宙线的周日变化与半日变化特征消失，在太阳活动低年逐渐向高年过度时，首先出现的是周日变化。半日变化特征出现要滞后于周日变化，22周太阳活动高年看不出周日变化，而23周太阳活动的高年周日变化非常显著，22周太阳活动的下降期。只有周日变化而无半日变化。这是分析北京宇宙线台近2个太阳活动周数据得到的新结果。     

Evidence of the radio-quiet hard X-ray precursor of the 13 December 2006 solar flare

We report multi-wavelength investigation of the pre-impulsive phase of the 13 December 2006 X-class solar flare. We use hard X-ray data from the anticoincidence system of spectrometer onboard INTEGRAL (ACS) jointly with soft X-ray data from the GOES-12 and Hinode satellites. Radio data are from Nobeyama and Learmonth solar observatories and from the Culgoora Solar Radio Spectrograph. The main finding of our analysis is a spiky increase of the ACS count rate accompanied by surprisingly gradual and weak growth of microwave emission and without detectable radio emission at meter and decimeter wavelengths about 10 min prior to the impulsive phase of the solar flare. At the time of this pre-flare hard X-ray burst the onset of the GOES soft X-ray event has been reported, positive derivative of the GOES soft X-ray flux started to rise and a bright spot has appeared in the images of the Hinode X-ray telescope (XRT) between the flare ribbons near the magnetic inversion line close to the sources of thermal and non-thermal hard X-ray emission observed by Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) during the flare. These facts we consider as evidences of solar origin of the increased pre-flare ACS count rate. We briefly discuss a possible cause of the pre-flare emission peculiarities.     

A nonlinear background removal method for seismo-ionospheric anomaly analysis under a complex solar activity scenario: A case study of the M9.0 Tohoku earthquake

A precise determination of ionospheric total electron content (TEC) anomaly variations that are likely associated with large earthquakes as observed by global positioning system (GPS) requires the elimination of the ionospheric effect from irregular solar electromagnetic radiation. In particular, revealing the seismo-ionospheric anomalies when earthquakes occurred during periods of high solar activity is of utmost importance. To overcome this constraint, a multiresolution time series processing technique based on wavelet transform applicable to global ionosphere map (GIM) TEC data was used to remove the nonlinear effect from solar radiation for the earthquake that struck Tohoku, Japan, on 11 March, 2011. As a result, it was found that the extracted TEC have a good correlation with the measured solar extreme ultraviolet flux in 26–34 nm (EUV_26–34) and the 10.7 cm solar radio flux (F_10.7). After removing the influence of solar radiation origin in GIM TEC, the analysis results show that the TEC around the forthcoming epicenter and its conjugate were significantly enhanced in the afternoon period of 8 March 2011, 3 days before the earthquake. The spatial distributions of the TEC anomalous and extreme enhancements indicate that the earthquake preparation process had brought with a TEC anomaly area of size approximately 1650 and 5700 km in the latitudinal and longitudinal directions, respectively.     

太阳质子通量模型研究

太阳质子事件对航天活动构成重要威胁, 预测一定时期内太阳质子通量对航天器抗辐射加固设计有重要的指导意义. 在第20至23太阳活动周的太阳质子事件数据统计分析的基础上, 建立了一个针对 E>10 MeV和 E>30 MeV太阳质子通量的新模型. 新模型与目前航天工程中常用的JPL模型相比较, 引入了太阳活动性对质子事件发生概率的影响因素, 能够评估不同太阳活动水平下的质子通量, 其结果更符合质子事件的分布特征.      

New evidence of solar variation in temperature proxies from Northern Fennoscandia

A new summer temperature proxy was built for northern Fennoscandia in AD 1000–2004 using parameters of tree growth from a large region, extending from the Swedish Scandes to the Kola Peninsula. It was found that century-scale (55–140 year) cyclicity is present in this series during the entire time interval. This periodicity is highly significant and has a bi-modal structure, i.e. it consists of two oscillation modes, 55–100 year and 100–140 year variations. A comparison of the century-long variation in the northern Fennoscandian temperature proxy with the corresponding variations in Wolf numbers and concentration of cosmogenic ¹⁰Be in glacial ice shows that a probable cause of this periodicity is the modulation of regional climate by the secular solar cycle of Gleissberg. This is in line with the results obtained previously for a more limited part of the region (Finnish Lapland: 68–70° N, 20–30° E). Thus the reality of a link between long-term changes in solar activity and climate in Fennoscandia has been confirmed. Possible mechanisms of solar influence on the lower troposphere are discussed.     

Equatorial Ionospheric Anomaly (EIA) and comparison with IRI model during descending phase of solar activity (2005–2009)

The ionospheric variability at equatorial and low latitude region is known to be extreme as compared to mid latitude region. In this study the ionospheric total electron content (TEC), is derived by analyzing dual frequency Global Positioning System (GPS) data recorded at two stations separated by 325 km near the Indian equatorial anomaly region, Varanasi (Geog latitude 25°, 16^/ N, longitude 82°, 59^/ E, Geomagnetic latitude 16°, 08^/ N) and Kanpur (Geog latitude 26°, 18^/ N, longitude 80°, 12^/ E, Geomagnetic latitude 17°, 18^/ N). Specifically, we studied monthly, seasonal and annual variations as well as solar and geomagnetic effects on the equatorial ionospheric anomaly (EIA) during the descending phase of solar activity from 2005 to 2009. It is found that the maximum TEC (EIA) near equatorial anomaly crest yield their maximum values during the equinox months and their minimum values during the summer. Using monthly averaged peak magnitude of TEC, a clear semi-annual variation is seen with two maxima occurring in both spring and autumn. Results also showed the presence of winter anomaly or seasonal anomaly in the EIA crest throughout the period 2005–2009 only except during the deep solar minimum year 2007–2008. The correlation analysis indicate that the variation of EIA crest is more affected by solar activity compared to geomagnetic activity with maximum dependence on the solar EUV flux, which is attributed to direct link of EUV flux on the formation of ionosphere and main agent of the ionization. The statistical mean occurrence of EIA crest in TEC during the year from 2005 to 2009 is found to around 12:54 LT hour and at 21.12° N geographic latitude. The crest of EIA shifts towards lower latitudes and the rate of shift of the crest latitude during this period is found to be 0.87° N/per year. The comparison between IRI models with observation during this period has been made and comparison is poor with increasing solar activity with maximum difference during the year 2005.     

关于IMF北向分量特强时的太阳风－磁层－电离层耦合

关于ＩＭＦ北向分量特强时的太阳风－磁层－电离层耦合沈长寿，资民筠（北京大学地球物理系，１００８７１）（中国艺术研究院，北京）关键词行星际磁场，太阳风－磁层能量耦合函数为检验Ａｋａｓｏｆｕ提出的能量融合函数“’在ＢＺ强北向时能否反映太阳风与磁层扰动间的...     

27-day variation in solar-terrestrial parameters: Global characteristics and an origin based approach of the signals

The Earth and the near interplanetary medium are affected by the Sun in different ways. Those processes generated in the Sun that induce perturbations into the Magnetosphere-Ionosphere system are called geoeffective processes and show a wide range of temporal variations, like the 11-year solar cycle (long term variations), the variation of ～27?days (recurrent variations), solar storms enduring for some days, particle acceleration events lasting for some hours, etc.In this article, the periodicity of ～27?days associated with the solar synodic rotation period is investigated. The work is mainly focused on studying the resulting 27-day periodic signal in the magnetic activity, by the analysis of the horizontal component of the magnetic field registered on a set of 103 magnetic observatories distributed around the world. For this a new method to isolate the periodicity of interest has been developed consisting of two main steps: the first one consists of removing the linear trend corresponding to every calendar year from the data series, and the second one of removing from the resulting series a smoothed version of it obtained by applying a 30-day moving average. The result at the end of this process is a data series in which all the signal with periods larger than 30?days are canceled.The most important characteristics observed in the resulting signals are two main amplitude modulations: the first and most prominent related to the 11-year solar cycle and the second one with a semiannual pattern. In addition, the amplitude of the signal shows a dependence on the geomagnetic latitude of the observatory with a significant discontinuity at approx. ±60°.The processing scheme was also applied to other parameters that are widely used to characterize the energy transfer from the Sun to the Earth: F10.7 and Mg II indices and the ionospheric vertical total electron content (vTEC) were considered for radiative interactions; and the solar wind velocity for the non-radiative interactions between the solar wind and the magnetosphere. The 27-day signal obtained in the magnetic activity was compared with the signals found in the other parameters resulting in a series of cross-correlations curves with maximum correlation between 3 and 5?days of delays for the radiative and between 0 and 1?days of delay for the non-radiative parameters. This result supports the idea that the physical process responsible for the 27-day signal in the magnetic activity is related to the solar wind and not to the solar electromagnetic radiation.