Measuring the position of the polarization plane of solar coronal emission during eclipse observations

We analyze the suitability of digital equipment with CCD arrays for polarization measurements of solar coronal emission during eclipses. The effect of errors in the method on the derived plane of polarization is estimated. In principle, precise measurements of the plane of polarization can be used to determine the amplitude and direction of the current of a heliospheric plasma sheet. The errors in ordinary nondigital photometric measurements (5%) are too large to enable the resolution of a number of problems having to do with the three-dimensional structure of the solar corona.     

On stereoimages of some structures in the solar atmosphere

Three-dimensional structures in the solar chromosphere and corona are considered. It is demonstrated that two photoheliograms separated by ～1 day can be used (using computer-graphics methods) to construct a stereo image of the Sun. The algorithm for this is presented and carried out for H_α images of the total disk. A bulge in the equatorial region resulting from the differential rotation of the Sun can be seen in the stereo image. Structures called Whitney pleats in catastrophe theory are observed in the solar corona. Such structures are encountered in prominences. The well-known helmets (or streamers) are pleats of heliospheric plasma sheets. Isophotes for such a sheet and the degree of polarization of the radiation in the pleat are calculated and compared with observational data.     

Solar modulation of galactic cosmic rays in the three-dimensional heliosphere according to meteorite data

Cosmogenic radionuclides with distinctive half-lives from chondritic falls were used as natural detectors of galactic cosmic rays (GCR). A unique series of uniform data was obtained for variations in the integral gradients of GCR with a rigidity of R > 0.5 GV in 1955–2000 on heliocentric distances of 1.5–3.3 AU and heliographic latitudes between 23° S and 16° N. Correlation analysis was performed for the variations in GCR gradients and variations in solar activity (number of sunspots, SS, and intensity of the green coronal line, GCL), the intensity of the interplanetary magnetic field (IMF), and the inclination of the heliospheric current sheet (HCS). Distribution and variations of GCR were analyzed in 11-year solar cycles and during a change in 22-year magnetic cycles. The detected dependencies of GCR gradients on the intensity of IMF and HCS inclination provided insight into the differences in the processes of structural transformation of IMF during changes between various phases of solar and magnetic cycles. The investigated relationships lead to the conclusion that a change of secular solar cycles occurred during solar cycle 20; moreover, there is probably still an increase in the 600-year solar cycle, which can be among the major reasons for the observed global warming.     

The increase in the magnetic flux from the polar regions of the Sun over the last 120 years

The latitudes of the zonal boundaries of the global magnetic field of the Sun are determined from the magnetic neutral lines on synoptic Hα maps obtained during 1878–1999. The area of the polar zone occupied by magnetic field of a single polarity at solar minima has doubled over the last 120 years. This provides an explanation for the secular increase in heliospheric characteristics, which differs from the two-fold increase of the magnetic field strength predicted for this period. The temporal variations of the magnetic flux from the polar regions and their role in global changes of the Earth’s climate are discussed in connection with secular variations in the structure of the internal magnetic field of the Sun.     

Long-term variations in the asymmetry of the magnetic field of the sun and heliosphere

The asymmetry of the magnetic field of the Sun and its manifestation in the interplanetary magnetic field (IMF) are studied. The dominant magnetic polarity of the radial component of the IMF alternates from cycle to cycle, but with an overall systematic dominance of polarity directed toward the Sun. The global asymmetry is also manifest in the component of the IMF perpendicular to the plane of the solar equator. The dominance of positive values of B _z together with an appreciable linear trend in the cumulative sum of this quantity is interpreted as a manifestation of a relic solar magnetic field. The strength of this relic magnetic field near the Earth is estimated to be 0.048 ± 0.015 nT, based on the growth of the linear component of the cumulative sum of B _z . Time intervals, in which negative values of the B _z component of the IMF dominate and enhanced geomagnetic activity is observed, are identified. Our analysis of solar and heliospheric magnetic fields in an integrated representation has enabled us to compare various types of measurements and estimate their stability.     

The phase shift between the hemispheres in the solar activity cycle

The shift between the solar activity cycles in the northern and southern hemispheres of the Sun is studied using data on sunspot number and area. The data obtained are compared with archival information on episodes of appreciable solar-cycle asymmetry. The small phase shift between recent activity cycles in the northern and southern solar hemispheres differs considerably from the shift for episodes of appreciable deviations from dipolar symmetry in the sunspot distribution detected with various degrees of confidence in archival astronomical data from the 17th–19th centuries. The current time shift between the hemispheres is insignificant, about 6–7 months. This shift has changed its sign twice in recent solar history; this probably corresponds to more or less periodic variations with a timescale close to the duration of the Gleissberg cycle.     

透射槽波相邻道质心频率的层析成像方法

槽波勘探是煤层工作面小构造探测的主要方法之一,该方法主要是利用槽波的能量衰减特征。当检波器的耦合差或工作面存在较大地质异常时,会显著影响槽波在不同频段上的能量分布,降低槽波探测结果的稳定性和准确性。利用槽波信号的质心频率变化特征进行反演成像是一种创新且有效的方法,但该方法存在震源质心频率准确估算及兼顾震源差异性的难题。为此,提出基于透射相邻道槽波信号,估算其质心频率相对变化量的层析成像方法。基于理论分析,推导出相邻道槽波质心频率相对变化量(M_i)的计算公式;采用二维数值模拟方法,验证槽波M_i值与传播距离的正向线性变化规律;通过槽波实测试验,对比分析了相邻道质心频率成像方法的效果。结果证明,槽波信号存在频移现象,槽波相邻道M_i值层析成像方法是有效,该方法克服了震源差异性和震源质心频率人为选择不当对成像结果造成的影响,为槽波勘探数据处理提供了一种新的思路。      

1991年初夏江淮大水的天文因素──太阳质子耀斑爆发

研究了1991年初夏江淮大水前,北半球环流的异常与太阳上的一系列质子耀斑之间的关系.研究结果表明:太阳上连续不断的质于耀斑爆发是1991年初夏江淮大水的重要天文因素.太阳质子耀斑可能触发或加剧了极涡的冷空气南下,低空西南急流的东移和西太平洋副热带高压的西伸北移过程.由于冷热气流多次在长江中下游和淮河地区相遇.因而形成了频繁的暴雨和特大暴雨过程,造成了江淮地区的特大洪涝灾害.     

Global solar magnetology and reference points of the solar cycle

The solar cycle can be described as a complex interaction of large-scale/global and local magnetic fields. In general, this approach agrees with the traditional dynamo scheme, although there are numerous discrepancies in the details. Integrated magnetic indices introduced earlier are studied over long time intervals, and the epochs of the main reference points of the solar cycles are refined. A hypothesis proposed earlier concerning global magnetometry and the natural scale of the cycles is verified. Variations of the heliospheric magnetic field are determined by both the integrated photospheric i(B _r )_ph and source surface i(B _r )_ss indices, however, their roles are different. Local fields contribute significantly to the photospheric index determining the total increase in the heliospheric magnetic field. The i(B _r )_ss index (especially the partial index ZO, which is related to the quasi-dipolar field) determines narrow extrema. These integrated indices supply us with a “passport” for reference points, making it possible to identify them precisely. A prominent dip in the integrated indices is clearly visible at the cycle maximum, resulting in the typical double-peak form (the Gnevyshev dip), with the succeeding maximum always being higher than the preceding maximum. At the source surface, this secondary maximum significantly exceeds the primary maximum. Using these index data, we can estimate the progression expected for the 23rd cycle and predict the dates of the ends of the 23rd and 24th cycles (the middle of 2007 and December 2018, respectively).     

用于岩体质量评价的地震波Q值计算方法

利用地震记录中的衰减信息(波形与频谱)计算岩体的品质因子(Q值),对岩体质量进行准确评价,典型的方法有振幅法、上升时间法、频谱比法、质心频率偏移法。本文介绍了这些方法的原理,并对它们的稳定性、适用情况做出了评价。     

On the origin of the low energy cosmic rays from stellar sources

The model of stellar origin of the anomalous component in the low energy cosmic rays for He to Fe ions observed in space vehicles is studied in the light of recent results. The model of heliospheric origin by Fisket al which has several attractive features cannot explain the long-term variations of intensity observed during 1974 to 1978 as pointed out by Nagashima and Morishita. The stellar origin model of Durgaprasad and Biswas, on the other hand, can easily account for the sudden appearance of the anomalous component in 1972 and its large decrease in intensity in 1978 on the basis of polarity reversal of the solar magnetic field as discussed by Nagashima and Morishita (1980). In this work, we show that in the stellar model energetic ions of He, C, N, O, etc. could originate in O-type stars which manifest very strong stellar wind with mass loss rate of 3·10^?6 M_⊙ per year. These have terminal velocities of about 1200 to 4000 km/sec and are typically a few times their escape velocity. These velocities correspond to ion energies of 10 to 100 keV/amu. These ions are in partly ionised state and are accelerated in the interstellar shock fronts to about 1 to 50 MeV/amu and thus account for the observed anomalous component of low energy cosmic rays.     

渗透系数的空间变异性对污染物运移的影响研究

随机水文地质学方法,较传统的确定性方法而言,是解决非均质含水层中水流和溶质运移问题的一种更为合理的手段。据以往研究,假设渗透系数场遵循对数正态分布,利用直接傅立叶变换方法来生成渗透系数随机场。应用基于随机理论的蒙特卡罗方法,来研究渗透系数的空间变异性对污染物运移结果的影响。实例研究表明,污染物在含水层中运移过程中污染羽的展布范围(二阶矩)随着渗透系数空间变异方差的增大而扩大,而污染羽在空间上的质心位置(一阶矩)基本不受方差的影响,仅取决于渗透系数随机场的均值大小。另外还分析了污染羽在各点的浓度变化方差和变异系数分别随渗透系数变异方差的变化状况。     

Variations of the dipole magnetic moment of the sun during the solar activity cycle

Observations of the large-scale solar magnetic field (synoptic maps) and measurements of the magnetic field of the Sun as a star (the total magnetic field) are used to determine the dipole magnetic moment and direction of the dipole field for three successive solar cycles. Both the magnetic moment and its vertical and horizontal components vary regularly during the cycle, but never disappear completely. A wavelet analysis of the total magnetic field shows that the amplitude of the 27-day variations of this field is very closely related to the magnetic moment of the horizontal dipole. The reversal of the global dipole field corresponds to a change in the inclination of its axis and occurs in a series of steps lasting one to two years rather than continuously. Before the onset of the reversal, the dipole axis precesses relative to the solar rotational axis, then shifts in a meridianal plane, reaching very low latitudes, where a substantial shift in longitude then begins. These results are discussed in connection with helioseismological data indicating the existence of oscillations with a period of about 1.3 yr and properties of dynamo processes for the case of an inclined rotator.     

Variations in the solar luminosity,radius, and quadrupole moment as effects of a large-scale dynamo in the solar convection zone

Astronomy Reports - The effect of large-scale magnetic fields generated by the solar dynamo on the irradiance of the Sun and stratification of the solar convection zone is studied using a numerical...     

基于VSP资料进行的吸收系数Q值反演

采用比较热门和精确的心迹线法实现利用地震VSP资料进行Q值反演。通过实例验算,证实了这种方法的可行性和有效性。在反演过程中,该方法对超过350 m的厚层反演效果较为准确,对薄层其反演效果不稳定,但总体趋势不会有大的变化。     

太阳活动驱动气候变化空间天气机制研究进展

大量研究表明，从数小时到十年、百年时间尺度上的天气、气候变化受太阳活动影响显著。近年来，全球云量、北大西洋冬季气旋等气候、气象要素与银河宇宙射线通量变化、太阳能量粒子事件等空间天气事件显著的统计相关被陆续发现。在此基础上，提出太阳活动驱动气候变化空间天气机制，其基本观点是：空间天气事件通过改变云物理特性影响气象、气候，其核心是：太阳活动造成的空间天气事件与云微物理过程的联系，目前空间天气理论分化为离子诱导成核机制和全球大气电路—静电云微物理机制（简称Tinsley机制）。主要回顾和总结了近年来空间天气机制研究的发展，包括观测与理论，取得的成果，并对其未来的发展提出展望。      

地形对黄河流域太阳辐射影响的分析研究

起伏地形中太阳总辐射由直接辐射、散射辐射、周围地形反射辐射三部分组成,依据各部分太阳辐射产生机理的不同,分别设计模型以综合考虑天文因素、大气因素、宏观地理因素、局地地形因素（坡向、坡度、地形相互遮蔽）是必须的。基于数字高程模型（DEM）数据和遥感影像,在全面考虑各种因素的基础上,建立了依托常规气象站观测资料的起伏地形下太阳总辐射计算模型,完成了黄河流域1km×1km分辨率太阳总辐射分布式模拟。结果表明：受坡地自身遮蔽和周围山地相互遮蔽的影响,总体平均而言,山地接收的太阳总辐射较平地少;局地地形对太阳辐射的影响程度随季节而变,在太阳高度角较低的季节,局地地形的影响较为显著。     

Solar forcing of the terrestrial atmosphere

The Sun provides the main energy input to the terrestrial atmosphere, and yet the impact of solar variability on long-term changes remains a controversial issue. Direct radiative forcing is the most studied mechanism. Other much weaker mechanisms, however, can have a significant leverage, but the underlying physics is often poorly known. We review the main mechanisms by which solar variability may impact the terrestrial atmosphere on time scales ranging from days to millennia. This includes radiative forcing, but also the effect of interplanetary perturbations and energetic particle fluxes, all of which are eventually driven by the solar magnetic field.     

降雨对青藏高原多年冻土区地表辐射的影响——以北麓河地区为例

青藏高原地表辐射变化影响多年冻土地表能量收支平衡、热工计算温度场边界条件以及冻土热稳定性。降雨变化是影响地表辐射的重要因素,以青藏高原北麓河地区的地表辐射资料和浅层地表水热监测数据为基础,分析了降雨对多年冻土区地表辐射特征的影响。研究表明：受降雨影响,辐射分量具有明显的日变化和年际变化特征,短波辐射被严重削弱,地面长波辐射削弱程度较低,而太阳长波辐射增强。小雨作用后,太阳短波、地面短波、地面长波辐射日积分量分别减少24.6%、37.9%、4.2%,太阳长波增加了4.3%;中雨作用后,太阳短波、地面短波、地面长波辐射日积分量分别减少32.2%、43.4%、1.7%,太阳长波增加了11.6%;大雨作用后,太阳短波、地面短波、地面长波辐射日积分量分别减少56.3%、65.5%、4.4%,太阳长波增加了10.7%;降雨作用后地表反照率减小,且呈不对称“U”形变化,地表净辐射增加,长期时间尺度上降雨对净辐射影响不明显;降雨对辐射特征的影响程度与降雨强度呈正相关且地表辐射对降雨变化的响应有滞后效应。在暖湿化背景下,冻土热工计算中应考虑降雨对多年冻土区地表能量平衡和水热边界的影响。     

Brecciation driven by changes in fluid column heights

A mechanism is presented for the pulses of high fluid pressure (P_F) necessary for fluid‐assisted brecciation. Establishment of hydraulic‐ or pneumatic‐connectivity between rock masses with different P_F can cause overpressure in the higher rocks because the P_F gradient is parallel to the hydrostatic gradient (the centroid effect). P_F can become high enough to create a fracture network, with an influx of fluids and mineralisation occurring as fluids migrate to areas of lower P_F. Changes in P_F caused by the centroid effect can cause other structures and seismicity.