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在磁化磁场为恒定磁场(无定向磁力仪─-A)与10kHz交变磁场(MiniseP旋转磁力仪─-M)的两种情况下,作岩样比测时发现,后者测得的主磁化率值кM较小,而且沿磁性叶理面方向f的主磁化率值кmax与кint比沿其法线方向n上的кint减少得更多.作者以涡流磁滞机构对磁性载体材料的“磁屏蔽”作用发生了各向异性的影响来解释此现象;并推测磁化率各向异性存在频散现象. 相似文献
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分析了北半球不同时域O3层遥相关型的空间结构及其演变特征,探讨了太阳活动和极涡振荡对O3层遥相关型形成和演变的作用.结果发现:1.O3层对太阳活动响应具有显著的区域性,在不同季节里只存在一种O3层遥相关型与其相联系,随着季节的转换大气环流与太阳活动效应叠加将使O3层的响应区域及遥相关型的空间结构发生转移现象.2.极涡增强将导致O3层出现负异常,且在遥相关区域中O3含量的振幅变化最为显著.由于极涡的不对称性,各分区极涡强度对O3层遥相关型的影响存在着显著差异,表明极涡形变对O3层遥相关型的形成和演变具有重要作用. 相似文献
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亚热带富铁土的磁学性质及其磁性矿物学 总被引:7,自引:3,他引:4
通过55个亚热带富铁土的磁化率(χ)、频率磁化率(χfd)、非滞后剩磁(ARM)和饱 和等温剩磁(SIRM)等磁性参数测定,结合氧化铁化学形态分析和矿物鉴定,初步明确了亚热 带富铁土的磁学特征及其磁性矿物.磁测数据表明富铁土中存在强磁性的矿物,其磁化率χ 与土壤游离氧化铁(Fed)含量呈极显著指数正相关(R2=0.5971),频率磁化率χfd与土壤游离氧 化铁含量呈极显著直线正相关(R2=0.4289).富铁土的χfd和非滞后磁化率χARM。值表明土壤 中的磁性矿物以超顺磁性(SP)和稳定单畴(SSD)颗粒为主,富铁上的χ和χARM呈极显著直线 正相关(R= 0.9429),证明富铁土的磁性是由风化成土过程产生的 SP和 SSD磁性颗粒贡献 的.矿物磁测结合X-衍射证明富铁土中的氧化铁矿物由赤铁矿、磁赤铁矿和针铁矿组成。 相似文献
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利用一个时变电离层理论模式,研究武昌地区(30.5°N,114.4°E)电离层F1-ledse现象.表明利用当前关于中性气体和太阳辐射的经验模式,观测到的F1-ledge出现与演化的基本规律将可基于现有电离层理论加以再现.指出较明显的F1-ledge结构同较低的中性原子-分子含量比有直接关系,并同原子-分子成份的过渡高度、背景温度及其垂直分布形态有一定联系.同F1-ledge形态相关联的F1-F2谷,其出现主要是由于亚稳态氧离子参与光化过程,以及电离气体参与具有一定垂直变化的输运过程. 相似文献
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在保证低频自由振荡信号分辨率,又不对高频自由振荡信号产生抑制效应的前提下,利用张家口地震台体应变观测资料,采用功率谱密度估计方法,获得2011年3月11日日本9.0级大地震激发的0S2-0S74基频球型振荡和17个谐频球型振荡(3S2、5S3、2S10、2S12、3S9、11S1、7S10、5S13、4S18、5S14、14S4、4S24、1S38、7S18、14S8、9S19、5S30),并与地球初步参考模型(PREM)的理论自由振荡周期进行对比,发现与实测振荡周期基本一致。 相似文献
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从Rankine-Hugoniot关系出发,以激波切向磁场ξ、上游激波角θ1和等离子体β1值为参数研究各类激波解的特性及相互关系,阐明各类激波强度随介质β值的变化规律.结果指出:(1)在ξ<-1的Ⅰb型中间激波区和ξ>4的快激波区存在双解;(2)慢激波可以直接和中间激波连接,但不能和快激波直接连接;(3)各类激波强度(用激波密度比衡量)随β1值均有变化:Ⅰb型中间激波上支随β1值增加而下降,下支则上升;Ⅰa型中间激波和慢激波都随β1值增加而下降;快激波双解区上支随β1值增加而下降。下支上升;快激波在1<ξ<4区间的解随β1值增加而上升。 相似文献
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稳定电流场反射和透射问题的讨论张金钟(西安石油学院,西安710061)在两种线性、各向同性媒质的分界面上,电力线会发生弯折,这是熟知的事实.如图三所示,两媒质的电阻率分别为P1和P2,入射电场Er和折射电场Et与界面法线方向的夹角分别为a和r.文献... 相似文献
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The velocities of the stationary extra-ecliptic solar wind are analyzed depending on the heliolatitudes, heliocentric distances,
and solar activity. An analysis has been performed using the direct measurements of the solar plasma flux velocities onboard
Ulysses and the simultaneous ground-based IPS observations. The arguments for the hypothesis that primary high-speed (V ∼ 900 km/s) flows exist at the corona bottom and are directly related to the photosphere and solar magnetic fields are presented.
The possible mechanism by which high-speed streams are generated is generally considered. 相似文献
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E. N. Parker 《地球物理与天体物理流体动力学》2013,107(3-4):161-182
Abstract The relatively large resistivity in the solar photosphere and chromosphere softens the ideal tangential discontinuities of magnetostatic equilibrium into continuous transitions in field direction over scales of 0.1–10 km. This softening is communicated upward at the Alfvén speed into the active solar corona. The degree of softening is a vital part of the theory of magnetic heat input to the active X-ray corona, because the very low resistivity of the coronal gas provides effective dissipation only if the current sheets are reduced to a thickness of 10?2km. A close examination of the problem shows that the Alfvén transit time up into the corona is large compared to the characteristic time of 1 sec in which the coronal tangential discontinutities are formed. It also shows that the principal effect of the resistivity is to create a thin surface layer of fluid on adjacent flux bundles, which causes a general drift of the flux but does not directly broaden the current sheets higher up in the field. In fact the motions of the surface layers do not extend upwards beyond the first winding pattern at each end of a coronal loop. It appears that the photospheric and chromospheric resistivity is without striking consequences for magnetic heating in the corona. 相似文献
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根据1995-1997年3年中山站数字式电离层测高仪的数据,分析了中山站不同季 节F层的临频变化特点.中山站夏季主要受太阳光光化电离的影响,F层临频随地方时的变 化与中纬台站相似;两分季,极隙区软电子沉降的作用显著,F层临频随磁地方时而变化,有 较明显的磁中午现象.冬季,太阳全天处于地平线以下,中山站F层临频的变化主要受极隙 区软电子沉降和极区等离子体漂移的影响,其峰值变化处于碰中午和地方时中午之间.中山 站夏季全天都能观测到F层的存在;两分季F层在地方时子夜附近的出现率较少;冬季月份 在磁地方时午后和子夜F层出现率明显减少,这可能与南半球冬季的高纬槽和极洞有关.对 F层不均匀区的分析认为,中山站在t_(LT)为16:00左右处于极光带赤道侧,20:00左右进入极盖 区。 相似文献
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五矩二流太阳风等离子体特性的数值研究 总被引:4,自引:0,他引:4
本文数值求解了各向同性二流太阳风的五矩方程组,得出了1 Rs-2AU区域内太阳风密度、速度、电子和质子温度、它们的热流通量密度q以及非麦克斯韦分布尾部粒子过剩量ξ随日心距离的变化关系.文中比较了二流太阳风五矩模型、四矩模型(ξ=0)和低阶矩模型(不包括q和ξ二个矩方程)的等离子体特性,着重讨论了量ξ对质子温度及其热流通量的影响.结果表明,包括言的五矩方程可改善Te/Tp和qe/qp的计算值与观测值的符合程度. 相似文献
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V. M. Grigoryev L. V. Ermakova I. I. Salakhutdinova A. I. Khlystova 《Geomagnetism and Aeronomy》2009,49(7):823-829
The dynamics of the magnetic field and velocity field during the birth and an early development stage of a major active region
is studied. SOHO MDI longitudinal-component magnetograms, Dopplergrams, and continuum images are used. The presence of an
enhanced material upflow in the photosphere during the passing of the top of the magnetic flux loop, forming the active region,
is revealed. The maximum upflow velosity is 2 km/s and the maximum size of the upflow area exceeds 20000 km. The lifetime
of the upflow is about two hours. The undulating form of the magnetic flux tubes crossing the photosphere is confirmed. A
structural-analysis technique is used to show that the trailing polarity field at the formation stage of the active region
is more highly structured than the leading polarity field. 相似文献
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G. N. Kichigin L. I. Miroshnichenko V. I. Sidorov S. A. Yazev 《Geomagnetism and Aeronomy》2016,56(4):393-400
The analysis of observations of large solar flares made it possible to propose a hypothesis on existence of a skin-layer in magnetic flux ropes of coronal mass ejections. On the assumption that the Bohm coefficient determines the diffusion of magnetic field, an estimate of the skin-layer thickness of ~106 cm is obtained. According to the hypothesis, the electric field of ~0.01–0.1 V/cm, having the nonzero component along the magnetic field of flux rope, arises for ~5 min in the surface layer of the eruptive flux rope during its ejection into the upper corona. The particle acceleration by the electric field to the energies of ~100 MeV/nucleon in the skin-layer of the flux rope leads to their precipitation along field lines to footpoints of the flux rope. The skin-layer presence induces helical or oval chromospheric emission at the ends of flare ribbons. The emission may be accompanied by hard X-ray radiation and by the production of gamma-ray line at the energy of 2.223 MeV (neutron capture line in the photosphere). The magnetic reconnection in the corona leads to a shift of the skin-layer of flux rope across the magnetic field. The area of precipitation of accelerated particles at the flux-rope footpoints expands in this case from the inside outward. This effect is traced in the chromosphere and in the transient region as the expanding helical emission structures. If the emission extends to the spot, a certain fraction of accelerated particles may be reflected from the magnetic barrier (in the magnetic field of the spot). In the case of exit into the interplanetary space, these particles may be recorded in the Earth’s orbit as solar proton events. 相似文献
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A long series of the known Π index of the solar corona structure has been proposed. It seems that this index, which characterizes the limb extension of polar coronal plume systems, is of importance because it is related to the large-scale polar solar magnetic flux. Solar corona photographs and drawings during total solar eclipses, collected for 13 solar activity cycles from different sources (78 eclipses), as well as H-alpha map data on the drift of the high-latitude belt of filaments before polarity reversal of the polar magnetic field have been used. Daily solar corona images, obtained on the SOHO spacecraft (using an EIT ultraviolet telescope), have been additionally used. 相似文献
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一、引言自海尔(G.E.Hale)提出太阳耀斑活动的特性为日地关系的重要关鍵这一問題后,近30年来天文学家、地球物理学家对于耀斑所引起的一系列的現象,进行了許多研究工作。爱立生(M.A.Ellison)曾将研究太阳耀斑本身及其所引起的地球物理現象等工作,就其性貭綜合为九个方面.其中联系到地磁方面的为与耀斑几乎同时发生的紫外綫輻射所引起的“鈎扰”,和由于耀斑发射出来的微粒子流在1-2天以后达到地球而引起的“磁暴”. 相似文献
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本文分析了1987年9月23日日环食期间,我国14个电离层站和1988年3月18日日全食期间两个站的垂测仪和偏振仪记录,并综合50年代以来历次日食电离层效应的观测结果,证实:1.E层和F1层光食效应明显,F2层动力学效应显著;2.f0F2存在日食日值大于、小于或等于控制日值三种典型情况;3.TEC食变曲线有凹陷和不凹陷两种典型情况,甚至出现日食日值大于控制日值的异常现象. 本文对F2层和外电离层的动力学特征作了定性讨论,认为:空间等离子体温度急剧下降和沿场扩散是F2层和外电离层日食效应的最主要因素;而磁赤道上空等离子体的沿场扩散、“喷泉”效应,热层风和全(环)食带方位是影响位于磁赤道异常区各电离层站日食电离层效应的主要因素. 相似文献