Relation between the active region magnetic field and solar flares

A weak active region (NOAA 11158) appeared on the solar disk near the eastern limb. This region increased rapidly and, having reached the magnetic flux higher than 10²² Mx, produced an X-class flare. Only weak field variations at individual points were observed during the flare. An analysis of data with a resolution of 45 s did not indicate any characteristic features in the photospheric field dynamics during the flare. When the flux became higher than 3 × 10²² Mx, active region NOAA 10720 produced six X-class flares. The field remained quiet during these flares. An increase in the magnetic flux above ～10²² Mx is a necessary, but not sufficient, condition for the appearance of powerful flares. Simple active regions do not produce flares. A flare originates only when the field distribution in an active region is complex and lines of polarity inversion have a complex shape. Singular lines of the magnetic field can exist only above such active regions. The current sheets, in the magnetic field of which the solar flare energy is accumulated, originate in the vicinity of these lines.     

Anisotropy of the horizontal velocity fluctuation field in the large wavenumber region

Mesoscale atmospheric wind, temperature, and density fluctuations are described in terms of their power spectra. In the early 1980s, VanZandt[1] showed that the observed spectrum of the atmospheric fluctuations can result, as in the ocean, from an interna…     

Anisotropy and symmetry of fluctuations in the solar wind magnetic field and velocity

The behavior of correlation tensors of fluctuations in the solar wind magnetic field and velocity is studied during different phases of a solar cycle on the basis of a 45-year measurement series of solar wind parameters. It is found that the orientation of fluctuations in the magnetic field and velocity is approximately axisymmetric relative to the direction of a local magnetic field during high solar activity. This symmetry is violated significantly during periods of low solar activity, and deviations from the symmetry are regular and oppositely directed during minima of even and odd 11-year cycles, which is probably connected with variations in the orientation of the Sun??s magnetic field. The dependence of the power of fluctuations on the local magnetic field direction reveals significant deviations from local symmetry during all phases of a solar cycle, especially for velocity fluctuations.     

近地等离子体片中磁场扰动和离子速度扰动的统计研究

利用THEMIS THC卫星观测数据统计分析近地等离子体片中磁场扰动和等离子体整体流的速度扰动的关系,研究Alfven波动的活动性.研究结果表明:1)等离子体整体流的速度扰动幅度依赖于平均速度的大小,速度扰动幅度随平均速度的增加而增加;2)速度扰动幅度与磁场扰动幅度存在较强的正相关性;3)磁场扰动幅度与AE指数密切相关,磁场扰动幅度随着AE指数增加而增加,而速度扰动幅度与AE指数之间没有明显的相关性;4)Alfven比与AE指数的相关系数较小,但能够看出Alfven比随着AE指数增加而减小的趋势;5)速度扰动幅度和磁场扰动幅度与尾向距离及距中性片距离的关系不明显.     

Phase variations of ULF magnetic field in the region of fault tectonics

The experiment on phase measurements of three components of a ULF magnetic field generated by a high-power controlled source in the region dominated by fault tectonics is described. The measurements were carried out along two orthogonal directions. It is established that the phase sharply varies by about 180° between some measurement points. The phase jumps are found to be confined to the conductive geological faults, which opens the possibility of locating the faults using the phases of ELF magnetic fields.     

二维位场在有源空间的解析延拓

位场的向下延拓对重、磁等位场资料的处理与解释具有重要意义,但现有的延拓方法在位场向下接近场源时会产生剧烈震荡,计算过程很不稳定,而且理论上都不能越过场源. 本文在复数域里定义了一个具有位场和几何双重特性的新函数PFGR,提出了一套新的延拓方法,在理论上实现了位场在包含场源的下半空间里的解析延拓,经过模型试算验证,表明该方法可以延拓越过场源,准确确定场源奇点,计算过程稳定,对测量中的随机噪声也具有较好的抗干扰能力.     

Nonlinear convection in an imposed horizontal magnetic field

Abstract

Nonlinear two-dimensional magnetoconvection, with a Boussinesq fluid driven across the field-lines, is taken as a model for giant-cell convection in the sun and late-type stars. A series of numerical experiments shows the sensitivity of the horizontal scale of convection to the applied field and to the Rayleigh number R. Overstable oscillations occur in cells as broad as they are deep, but increasing R leads to steady motions of much greater wavelength. Purely geometrical effects can cause oscillation: this work implies that strong horizontal field will in general lead to time-dependent convection.     

Evolution of the Tharsis region of Mars: insights from magnetic field observations

Mars Global Surveyor (MGS) observations of crustal magnetic fields over Tharsis provide new constraints on models for the thermal and magmatic evolution of this region. We analyze the distribution of magnetic field anomalies over Tharsis surface units of Noachian, Hesperian and Amazonian age. These data suggest that early Noachian crust underlies the Tharsis province, and formed contemporaneously with the existence of a martian dynamo. This crust either pre-dates the formation of Tharsis, or formed during the earlier phases of Tharsis volcanism. The preservation of strong magnetic field anomalies over some of the earliest Noachian and topographically high units, together with the observation of magnetic field anomalies over Hesperian- and Amazonian-age surface units, indicate that a large fraction of the magnetized crust has remained cool (below the blocking temperature of the magnetic carrier) throughout the construction of Tharsis. Moreover, the distributions of magnetic anomaly amplitudes over Noachian, Hesperian, and Amazonian surface units suggest that the youngest units overlie sites of prolonged intrusion and have undergone a greater extent of thermal demagnetization. The absence of magnetic anomalies around the Tharsis Montes and Olympus Mons argues for strong, localized heating, as would be expected at volcanic centers. We show that end-member models for progressive thermal demagnetization of a Noachian magnetized crustal layer are consistent with the anomaly amplitude distributions. We integrate the magnetic field observations with constraints from tectonics, gravity, and topography, and present a revised scenario for the evolution of the Tharsis region.     

Temporal and spatial correlations of the strain field in tectonic active region,southern Kyusyu,Japan

The southern Kyusyu district is one of the most characteristic subduction zones in Japan. In this region, large earthquakes occurred sequentially, although earthquake mechanisms are different and the distance between earthquakes is far. We investigate strain propagation caused by a strain fluctuation related to subducting plate velocity. For this purpose, we used the data obtained from extensometers installed in an observation network at Kyusyu district and applied the cross-correlation function. If the strain associated with the subduction propagates in the crust, it is expected that the correlation around arrival of propagating signal varies from steady state. The results suggest existence of strain propagation in the overlying crust. Its velocity is estimated to be about 90–140 km/year with a direction from the subduction zone to inland.     

日面方位磁场扰动和行星际磁场螺旋结构

文采用球坐标下2.5维理想MHD模型,对日球子午面内方位磁场扰动的传播进行数值模拟,重点分析它对行星际磁场螺旋角的影响. 本文认为,观测到的行星际磁场螺旋角大于Parker模型的预言值,是太阳表面不断向行星际发出同向方位磁场扰动的结果;太阳较差自转在太阳内部产生的方位磁场为这类扰动提供了源头. 模拟结果表明,采用持续时间等于周期的十分之一、扰动幅度为103nT量级的正向方位磁场扰动,就可使1 AU处行星际磁场的螺旋角增加2°左右,与有关观测结果相符. 模拟结果还表明,上述方位磁场扰动对日球子午面内的太阳风特性和磁场位形的影响基本上可以忽略.     

昆仑山口西8.1级地震前后山西及邻区速度场和应变场的变化

在山西及邻区,1999~2004年几乎所有的GPS站速度都小于1999~2001年,鄂尔多斯西部大多数GPS站1999~2004年的运动方向相对于1999~2001年发生了逆时针旋转。鄂尔多斯和山西中南部的NWW向运动与昆仑山口西8.1级大震断裂带以北地区的运动方向是一致的,而鄂尔多斯以南的向东运动与断裂带以南地壳的运动方向也是一致的。鄂尔多斯的逆时针旋转形成了109.0°E以西地区E-W方向的压应变。而它的逆时针旋转和太行山东部的向东伸展运动形成了109.0°E以东地区E-W方向的张应变。鄂尔多斯东部和山西地区在8.1级大震后的增量应变场减弱了基本应变场E-W方向压应变的积累,而鄂尔多斯西部的增量应变场增加了E-W方向压应变的积累。     

华北中部岩石圈磁场变化与岩石圈结构间的关系

对2016—2019年华北中部地区（34.7°—41.1°N,110.3°—119.7°E）流动地磁矢量观测数据进行处理,得到连续3期岩石圈磁场年变化数据,并对岩石圈磁场空间分布形态进行分析。研究发现,磁异常分布与岩石圈结构之间有一定相关性,在太行山隆起以西、临清坳陷、鲁西断隆和鲁西断隆以东等主要结构单元表现出不同程度的差异性,但在各自单元内却呈现出较好的整体性,岩石圈磁场水平矢量H和东向分量ΔY要素分区特征较明显。从H矢量空间分布形态可以看出,高能量区多分布在太行山隆起以西和鲁西断隆周边。文水—日照ΔY要素剖面幅值变化形态与结构分区间对应较好,对主要结构单元ΔX、ΔY、ΔZ要素异常幅度均值和极值进行统计,结果表明,太行山隆起以西近期岩石圈磁场变化幅度最大,异常能量最强,其次为鲁西断隆及以东地区,而临清坳陷周边磁场变化相对较平稳。     

Rayleigh-wave group velocity distribution in the Antarctic region

We determined 2D group velocity distribution of Rayleigh waves at periods of 20-150 s in the Antarctic region using a tomographic inversion technique. The data are recorded by both permanent networks and temporary arrays. In East Antarctica the velocities are high at periods of 90-150 s, suggesting that the root of East Antarctica is very deep. The velocities in West Antarctica are low at all periods, which may be related to the volcanic activity and the West Antarctic Rift System. Low velocity anomalies appear at periods of 40-140 s along the Southeastern Indian Ridge and the western part of the Pacific Antarctic Ridge. The velocities are only slightly low around the Atlantic Indian Ridge, Southwestern Indian Ridge, and the eastern part of the Pacific Antarctic Ridge, where the spreading rates are small. Around two hotspots, the Mount Erebus and Balleny Islands, the velocity is low at periods of 50-150 s.     

火星感应磁场模型及其磁力线分布

本文利用火星具有电离层而无内禀磁场的特点以及它与太阳风相互作用的性质,通过适当的假设,建立了火星感应磁场模型.此模型建立如下,利用电流连续的特性: Δ·j=0 (j为感应电流)以及对火星磁层中的电流体系分布的合理假设给出电流,并由毕奥—萨伐尔定理得到火星周围的磁场强度的表达式;利用我们自编的磁力线跟踪程序由求得的磁场强度得到火星周围的磁力线分布.我们发现:利用此火星磁场模型得到的火星周围的磁力线分布与卫星观测的结果以及其他方法得到的结果符合的很好.     

Peculiarities of the magnetic flux emerging in the equatorial solar zone

The magnetic flux longitudinal distribution in the equatorial solar zone has been studied. The magnetic synoptic maps of the Wilcox Solar Observatory (WSO) during Carrington rotations (CRs) 2052–2068 in 2007 and early 2008 have been analyzed. The longitudinal distributions of the area of the zones where the photospheric magnetic field locally enhanced have been constructed for each CR. The obtained distributions indicate that the zones are located discretely and that a clearly defined one narrow longitudinal interval with the maximum flux is present. The longitudinal position of this maximum shifted discretely by ≈130° at an interval of 5.5 ± 0.5 CRs. A longitudinal shift of the zones with an increased magnetic flux multiple of 60° was observed between the hemispheres. In addition, a time shift of ≈2.5 CRs existed between the instants when the position of maximum fluxes in different hemispheres shifted. The established peculiarities of the magnetic flux longitudinal distribution and time dynamics are interpreted as an action of supergiant convection cells. These actions result in that magnetic fields are removed from the generation region through the channels that are formed between such cells at a longitudinal interval of 120°. The average synodic rotation velocity of the considered equatorial channels, through which the magnetic flux emerges, is 13.43° day^–1.     

On longitudinal vibration of an elastic bar in a magnetic field

Summary The equations of elasticity, electromagnetic equations of Maxwell have been applied to investigate the longitudinal vibration of a partly homogenous, partly inhomogeneous elastic bar permeated by a magnetic field.     

张北6.2级地震前后地震波速比在源区与场区的变化特征

计算了 1 991年～ 1 999年发生在北纬 3 9°0 0′～ 42°0 0′,东经 1 1 2°3 0′～ 1 1 6°0 0′范围内的ML≥ 2 .0级地震的波速比 ,分析了张北 6 .2级地震前后源区与场区波速比的时空变化特征及其差异 ,发现 6 .2级地震前源区和场区波速比在时间分布上都出现较明显的低值异常 :下降—低值—平静—恢复—发震过程。在空间分布上低值异常比较集中和同步。对计算结果进行了 t检验 ,源区与场区波速比的时空变化及 t检验表明 6 .2级地震前源区与场区波速比异常非常明显 ,场区 1 995年开始出现波速比在正负之间比较大的变化后持续低值。 6 .2级地震后源区和场区的波速比计算结果一致 ,时空变化均为正常