PIC16F877A在新型质子旋进磁力仪中的应用

受制于当时微电子技术的发展,传统质子磁力仪存在电路复杂、元器件分立过多等不足之处,在确保观测原理不变的情况下,选取PIC16F877A作为主控芯片应用于新型质子旋进磁力仪中。介绍了整体的硬软件设计,同时与加拿大GEM公司生产的DiDd三分量磁力仪测量数据进行比较,结果显示在测量精度及准确度上两者非常接近,新型质子旋力进磁仪具有很好的稳定性和抗干扰性,达到了预期的效果。     

Comparing the latitudinal distribution of the <Emphasis Type="Italic">Pc</Emphasis>1 intensity and the position of subauroral proton spots

The latitudinal position of subauroral proton spots (special proton auroras observed from the IMAGE satellite) has been compared with the Pc1 pulsation intensity distribution determined using the data from the Finnish meridional network of induction magnetometers. It has been indicated that a Pc1 intensity maximum is always observed at the station that is closer to the proton aurora projection. Two Pc1 bands were registered in the event when two proton auroral spots were simultaneously observed at different latitudes. In this case, the Pc1 intensity distribution maximum at lower frequencies was related to a proton auroral spot at a higher latitude and vice versa. Such a spatial correlation between Pc1 pulsations and proton auroral spots, together with the previously established time correlation between these phenomena, demonstrates that subauroral proton spots reflect the region of ion cyclotron instability in the equatorial magnetosphere at the level of the ionosphere.     

锡林浩特地震台地磁观测干扰分析

对内蒙古自治区锡林浩特地震台2019年10-11月质子矢量磁力仪FHD-2B的数据进行常规分析,发现D分量测值数据出现噪声大、突跳多的异常现象。对该台质子矢量磁力仪受干扰数据进行傅里叶变换和小波分析,确定干扰源范围,排除外界干扰可能。进一步对仪器进行检测,确定干扰原因为参数漂移,在进行参数校正后,观测数据恢复正常。     

Relation between sudden increases in the solar wind dynamic pressure,auroral proton flashes,and geomagnetic pulsations in the Pc1 range

The interrelation between sudden increases in the solar wind dynamic pressure, auroral proton flashes on the dayside equatorward of the oval, and geomagnetic pulsations in the Pc1 range is considered on the basis of simultaneous observations of the solar wind plasma parameters, proton auroras on the IMAGE satellite, and geomagnetic pulsations at the Lovozero Observatory. It is indicated that proton luminosity flashes were observed in 70% of cases equatorward of the auroral oval during sudden changes in the solar wind pressure. In this case, flashes of proton auroras were observed in 85% of cases during sudden changes in the pressure, which were related to interplanetary shocks. Increases in pressure during tangential discontinuities were accompanied by flashes of proton auroras only in 45% of cases. When the ground station was conjugate to the region occupied by a proton aurora flash, the appearance or intensification of existent pulsations in the Pc1 range was observed in 96% of cases. When the ground station was not conjugate to the region of a proton luminosity flash, the response in geomagnetic pulsations was observed in 32% of events. When a sudden change in the solar wind pressure was not accompanied by a proton luminosity flash, the response in pulsations in the Pc1 range was hardly observed.     

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.     

Alfven脉动串级加热加速太阳风的二元流体模型

为研究太阳风的加速及加热机制，本又提出计算太阳风加速与加热的二元流体模型．该模型是建立在涂传治等提出的Alfven脉动的波能本级理论的基础上的．它能够描述从1Rs到1AU空间范围内太阳风的加速与加热，特别是它能够描述Alfven脉动的主要特性和Helios卫星对0.29－IAU空间范围内太阳风高速流的观测．上述结果说明Alfven波对太阳风的加速和加热有着十分重要的作用，并为研究太阳风的起源提供理论依据．     

核旋仪探头高度的探讨

本文根据试验观测结果,探讨了核旋仪探头高度改变对野外流动地磁场总强度观测质量的影响。认为适当提高探头高度,可以有效地消除地表物质不均匀磁性所带来的随机干扰。具体的探头高度可由不同工作区域的试验工作加以确定。     

太阳质子事件期间内辐射带质子通量的变化

本文介绍风云一号（B）卫星上的宇宙线成份监测器,在1991年1月30日及31目的耀斑期间及其前后几天,对能量在4-23MeV内的内辐射带质子通量的观测结果,并对这些结果做了详细的分析.结果表明,在这两次耀斑及其所产生的太阳质子事件期间,内辐射带质子通量有显著的变化:在磁漂移壳参量L≥1.64的空间,质子通量显著增强,增幅在40％-200％之间;在L=1.30-1.60的空间,质子通量的增强也较为明显,增幅在20％以上;总的变化趋势是,L越大的地方,质子通量的增强就越显著.质子事件之后,内辐射带质子通量又逐渐回复到质子事件之前平衡结构时的水平.     

新疆且末地磁基准台场址勘选

对拟建设的新疆且末地磁台进行场址勘选,采取十字剖面测量和密跨度测量方法进行地磁场总强度F测量,对测量结果进行初步分析.分析结果表明,且末地磁台的地质条件、磁场梯度分布和背景噪声环境等地磁观测环境条件,符合国家地磁台建设规范的要求,适宜地磁基准台站建设.     

Proton transport model in the ionosphere. 2. Influence of magnetic mirroring and collisions on the angular redistribution in a proton beam

We investigate the influence of magnetic mirroring and elastic and inelastic scattering on the angular redistribution in a proton/hydrogen beam by using a transport code in comparison with observations. H-emission Doppler profiles viewed in the magnetic zenith exhibit a red-shifted component which is indicative of upward fluxes. In order to determine the origin of this red shift, we evaluate the influence of two angular redistribution sources which are included in our proton/hydrogen transport model. Even though it generates an upward flux, the redistribution due to magnetic mirroring effect is not sufficient to explain the red shift. On the other hand, the collisional angular scattering induces a much more significant red shift in the lower atmosphere. The red shift due to collisions is produced by < 1 -keV protons and is so small as to require an instrumental bandwidth <0.2nm. This explains the absence of measured upward proton/hydrogen fluxes in the Proton I rocket data because no useable data concerning protons < 1 keV are available. At the same time, our model agrees with measured ground-based H-emission Doppler profiles and suggests that previously reported red shift observations were due mostly to instrumental bandwidth broadening of the profile. Our results suggest that Doppler profile measurements with higher spectral resolution may enable us to quantify better the angular scattering in proton aurora.     

同江地磁台勘选结果

依据GB/T19531.2—2004地震台站观测环境技术要求第二部分电磁观测,及DB/T9—2004地震台站建设规范(地磁台站)相关要求,应用G856质子旋进磁力仪,对拟建设的黑龙江省同江地磁台观测场地,采用30km十字剖面跨度测量和场地200m×200m、100m×100m密跨度方法进行勘选测量,通过对测量结果的分析,给出勘选结论和建议。     

漠河地磁台初步勘选结果

介绍了对拟建设的黑龙江省漠河地震台地磁观测场地进行的勘选,应用G856质子旋进磁力仪,采取十字剖面测量和200 m×200 m的密跨度(梯度)测量的方法,进行地磁场总强度F测量。经过对测量结果进行计算和初步分析处理后,认为:该场地适宜地磁台站建设。但是,如果确定在此建设地磁观测台站,还应按相关的规范和标准,进行深入的、详细的勘测。     

Energetic proton precipitation related to ion–cyclotron waves

This brief review summarizes recent findings related to particle precipitation associated with electromagnetic ion–cyclotron (EMIC) waves seen on the ground as geomagnetic Pc1 and IPDP pulsations.Particle precipitation signatures of ion–cyclotron interaction are described as revealed from low-altitude satellite measurements of the energetic proton fluxes as well as from observations of the proton aurora. As a result, localized proton precipitation patterns situated equatorward of the isotropy boundary are disclosed. One of the patterns is a proton precipitation spot in the morning sector, presumably mapped onto plasmapause; another one is an elongated region of the precipitation, presumably mapped onto the plasmaspheric plume.Clear evidence of the pitch-angle scattering associated with the ion–cyclotron wave activity is found near the equatorial plane in the region conjugated with the localized proton precipitation at low altitude.Thus, the revealed precipitation patterns determine the location of the region of intense pitch-angle scattering of energetic protons, and, therefore, their observations can be used to monitor the region of the ion–cyclotron interaction and to study its origin and properties. Some examples of such application of the low-altitude observations of energetic particles are described.     

Proton Auroras Equatorward of the Oval as a Manifestation of the Ion-Cyclotron Instability in the Earth’s Magnetosphere (Brief Review)

Different types of proton auroras observed by the IMAGE satellite equatorward of the proton aurora oval are briefly reviewed. These auroras are caused by the precipitation of energetic protons from the Earth’s magnetosphere during the development of the ion-cyclotron instability. In addition to the previously considered types of proton auroras (spots, evening arcs, and dayside flashes), a new type is described: longlasting proton auroras on the dayside. The scheme of interrelation between different proton auroras equatorward of the oval with the distribution of cold plasmaspheric plasma is given.     

Doppler-shifted auroral H <beta> emission: a comparison between observations and calculations

Two sounding rockets equipped with photometers and particle detectors have been flown into proton auroras. The measured altitude dependence of the proton flux is compared with calculations based upon known energy-range relations for protons in air. Expressions suitable for numerical calculations of Doppler profiles at arbitrary angles to the geomagnetic field and at different heights within an aurora are developed. Profiles due to some typical proton spectra have been calculated and it is shown that altitude profiles at some wavelengths are more sensitive to the shape of the proton spectrum than are profiles at other wavelengths. Variations in the H <beta> Doppler profile versus height for several angles with the magnetic field is studied. Profiles, as generated by the actually measured protons in the energy range 1 keV to 1 MeV, have been calculated and are compared with direct optical measurements made by ground and rocket photometers. The rocket photometers took measurements at different wavelengths within the Doppler profile. The correspondence between calculations and measurements is generally good. The total H <beta> is calculated and fair agreement with the measured intensity is found.     

太阳质子事件、双带耀斑及日冕物质抛射

本文统计了第２２ 太阳活动周期间（１９９１ ～１９９５ 年） 发生的２５ 个太阳质子事件与太阳耀斑及日冕物质抛射（ＣＭＥ） 事件的关系　　统计结果表明, 所有的太阳质子事件都与耀斑发生相关, 除２ 个质子事件（１９９４１０２０ 和１９９５１０２０ 日发生的太阳质子事件） 与ＣＭＥ发生无关, 其余质子事件也都与ＣＭＥ 相关　　值得注意的是, 与质子事件相关的耀斑有１６ 个是双带耀斑, 其中包括与ＣＭＥ无关的２ 个事件的耀斑, 占总数的６４ ％ 　　上述统计结果证实了无论是太阳耀斑, 还是物质抛射, 它们对太阳质子事件的发生同样起着非常重要的作用     

高能质子能谱特征在日冕物质抛射影响预报中的应用

日冕物质抛射(CME)的规模和对地有效性是地磁暴预报中重点关注的特征.本项研究的目的是通过对行星际高能质子通量和能谱的特征与演化规律的分析,得到CME对粒子的加速能力,评估CME可能对地磁场造成的影响.在工作中,统计分析了ACE/EPAM的1998-2010年的质子数据,对质子能谱进行了拟合,得到了能谱指数,并对能谱指数及其变化特征所对应的CME和地磁暴进行了相关统计.通过研究发现:(1)能谱指数随着太阳活动水平而变化,高年最大,达到-2.6,而且涨落幅度也达到±0.4,而在太阳活动低年则稳定在-3.0左右;(2)CME对粒子的加速对应着能谱指数的升高,幅度达到20%时,CME引起地磁暴的可能性较大;(3)冕洞高速流到达地球时,高能质子通量也会升高,但能谱指数同时会有下降;(4)以2004年全年的能谱指数为例,对能谱指数在地磁暴预报中的应用进行了评估,结论认为,能谱指数的升高是CME引发地磁暴的必要条件,可以作为地磁暴预报的参数使用.     

总强度在地震磁效应观测中的有效性

质子旋进磁强计(PPM)作为地磁场总强度标量测量的仪器, 具有稳定、操作简便、测量迅速等优点.其性能很适于地震磁现象的观测.可是, 总强度在震磁现象观测中是否有效, 中外从事此项研究工作的学者看法不一.本文以区分局部地磁异常的源场公式为基础, 论证了在地表地震磁异常的全域内, 总强度的变化不能为零, 其变化幅度ΔF与垂直分量的变化幅度ΔZ应大体相当, 这与实际震例和地震磁效应模型计算结果相吻合.这就使我们有可能充分利用PPM 作为总强度标量测量仪器的优越性, 在重点地区布署以总强度测量为主的台站和流动测网, 以尽力捕捉地震磁现象时空变化的全过程.      

Position of proton precipitation during auroral intensifications

The unique spectrographic observations of auroras on the Kola Peninsula, simultaneously performed in 1970 at Loparskaya and Kem stations using C-180-S cameras, have been analyzed by up-to-date digital data processing. The position and dynamics of proton precipitation relative to other manifestations of auroral and substorm activity (auroral arcs and electrojets) under moderately and weakly disturbed conditions have been analyzed. Several previously known regularities in the morphology of proton auroras have been confirmed. It has been indicated that the direction of motion of the proton band equatorward boundary in the evening sector changes at a sign reversal of the IMF Z component. Weak breakups affect the poleward boundary of the proton band but do not influence the position of the equatorward boundary of this band, which results in the expansion of the proton emission region. When a disturbance is stronger, the proton emission disappears near an active electron arc and subsequently appears poleward of its position before intensification. Short-term proton precipitation is also observed in the region of active electron precipitation during an intense breakup in the form of N–S structures.     

NOAA系列卫星高能粒子数据一致性统计分析

顶部电离层是低轨道卫星的运行空间,是能量粒子沉降的重要区域,认识这个空间的能量粒子分布特征对研究各种空间天气事件、地震、火山以及其他人类活动引起的扰动具有重要的现实意义.本文利用位于顶部电离层的5颗NOAA系列卫星数据,统计研究了100～300keV的电子和80～2500keV的质子的全球分布特征.研究发现:高能电子和质子主要分布在两极辐射带和南大西洋异常区,两极辐射带观测到的高能电子通量比南大西洋异常区高几倍到一个数量级,而质子则相反;高能电子在两极辐射带地区通量分布具有不对称性,主要表现为在北辐射带西经75°到东经90°存在低值区,相对应的是粒子主要聚集在其磁共轭区,且其边界和南大西洋异常区相交;高能质子两极辐射带对称分布,在南半球东经0°至东经50°存在高值区.利用概率密度统计分析发现,各颗卫星在南大西洋异常区和两极辐射带的高能电子和高能质子通量总体上均呈正态分布.在南大西洋异常区,NOAA-15观测到的高能电子通量比其他卫星的低,NOAA-16观测的高能电子通量比其他卫星的高,各卫星的高能质子观测结果基本相同.在两极辐射带,各卫星观测的高能电子通量结果基本相同,NOAA-18和...