太阳能量(或动量)是地壳运动的力源

目前多数地球科学家认为,地球的化（包括地壳运动和地震活动）是由地球内部因素决定的,地球外部因素是次要的,地球虽是庞大并具确定边界的星体,但从银河系看来,地球不能作为单独的星体存在,它必须依附太阳系才能生存下去,因此,研究太阳活动、太阳能量的向地球的输送及太阳与地球间能量（包括运量和质量）相耦 的物理机制,是研究地球演化的具体途径,应用地壳“轧展”效应理论,对地壳运动的成因及地壳内部的应力积累进行了     

后记之一

空间科学技术的蓬勃发展 ,特别是各类应用卫星对地球的观测、空间探测器对太阳活动的系统探测和对月球及行星的全面而综合的勘测 ,以及天体化学和比较行星学研究的兴起 ,大大扩展了人类的视野。借助于空间探测的成就 ,也即在更大的时空尺度上来研究地球生态环境的变化 ,并深化对全球变化的认识 ,已经成为一种必然的发展趋势。太阳活动是引起太阳系空间和地球环境变化及扰动的主要控制因素 ,太阳活动以巨大的能量和物质抛向地球 ,引起空间环境发生长期持续性变化和短期灾害性影响 ,给人类活动带来巨大损失。“蓬勃发展的空间天气学”、“‘地…     

地球物理学"九五"重大重点项目的布局及思考

1 "九五"重大重点项目的布局及思考 地球物理学是通过对地球的各种物理场(地震波、重力、磁、电、热等)的观测和研究来认识地球,是固体地球科学中吸纳高新技术能力最强的一个分支学科.空间物理学是把日球作为一个系统,研究太阳、太阳风同行星、慧星的上层大气、电离层、磁层、高能量粒子、其它星际物质间的相互作用.进入90年代以来,随着空间探测技术的发展和全球宽频带数字地震台网的建立等探测技术的进步,地球物理学和空间物理学步入了一个新的发展时期.这个发展时期的主要特点是:人们跨越时间界限,全方位的、定量的观察地球及其外围空间的各种过程,包括地球系统各层圈相互耦合和作用过程、动力学过程、非线性物理过程等.从而要求将地球物理学和空间物理学的研究层次提高到一个新的高度.     

基于小波分析的全新世气候千年周期及其成因

根据北大西洋、亚洲和热带大洋典型的全新世气候记录,采用小波分析方法建立太阳活动与地球气候之间的联系,揭示了过去9000年,太阳活动千年周期能量传递存在一个逐级(能级A,B和C)递减的过程.其中,北大西洋冰漂碎屑事件与太阳活动的相位差最小,揭示了由太阳活动驱动的冰漂事件是地球气候变化的起始点.在冷暖期转化过程上,亚洲石笋...     

行星地理学

行星地理学是研究地球、月球及太阳系九大行星运动特性对自然地理过程的影响的科学,它研究上述运动特性对大气、海洋及河流水文的影响,从而研究整个自然地理环境的变化。它是涉及天文、地球物理及自然地理诸要素(气候、水文与海洋等)的交叉学科。其主要理论基础为地球物理学,而研究方法则主要包括地球物理学、大气和海洋动力学、统计学及数值模拟等方面。国际上一些著名的地球物理及气候学家研究了这个问题,并取得了显著的进展,其代表人物是和Hunt。在我国,这方面的研究也处于世界前列,代表作者是彭公炳和任振球,前者主要研究地球自转速度变化和地极移动对气候、海洋和水文等自然地理条件的影响,其代表作是《气候的第四类自然因子》一书;后者主要研究月球及九大行     

对高精度重力测量中的固体潮校正的看法

固体潮是在月球和太阳引力作用下地球的形变现象。这个形变与整个地球都有关,即整个地球都在上述引力作用下产生不同程度的形变。这种理论近一、二十年才引起人们的注意。随着电子计算机的广泛使用,以及多门学科如天文学、海洋学、地球内部物理学、构造学、重力测量、地震学等的发展,固体潮研究也得到促进。      

地球物理学中的分形与分维研究进展

应用分形理论来研究地球物理现象,是近年来地球物理学研究中的新方法和新思路。本文介绍了分形与分维的基本概念,并综述了地球物理学中分形研究的最新进展。     

太阳辐射与气候变化

本文评述了太阳辐射改变对地球气候变化的影响,特别讨论了太阳活动,地球轨道参数和同太阳辐射有关的天文灾变等对气候不同时间尺度变化的影响。     

HOLOCENE CLIMATE MILLENNIUM CYCLE AND CAUSES BASED ON WAVELET ANALYSIS

根据北大西洋、亚洲和热带大洋典型的全新世气候记录,采用小波分析方法建立太阳活动与地球气候之间的联系,揭示了过去9000年,太阳活动千年周期能量传递存在一个逐级(能级A,B和C)递减的过程.其中,北大西洋冰漂碎屑事件与太阳活动的相位差最小,揭示了由太阳活动驱动的冰漂事件是地球气候变化的起始点.在冷暖期转化过程上,亚洲石笋与格陵兰冰芯呈现相反的模式,即是亚洲弱季风事件滞后而强季风事件超前;格陵兰冰芯冷期超前而暖期滞后.其机制可能是北欧淡水注入放大了弱太阳活动能量,导致亚洲季风强事件直接受太阳活动驱动,弱事件则响应于冰漂事件.     

生态地质条件评估的方法、原理和标准

文中确定了“生态地质条件”及“生态地质条件的现状”等术语的意义 ;阐述了用于评估生态地质条件的方法、原理以及标准和指标的分类 ;论述了地球动力学和地球物理学的标准和指标     

蓬勃发展的空间天气学

日地空间环境是人类生存发展的重要场所,太阳剧烈活动引起日地空间短时间尺度的变化,对人类社会带来严重影响和危害。本文简要介绍了空间天气学产生的背景和迅速发展的社会需求,当今国际合作研究的重大计划和进展,以及空间天气学研究的未来和展望。     

A study on precursors leading to geomagnetic storms using artificial neural network

Space weather prediction involves advance forecasting of the magnitude and onset time of major geomagnetic storms on Earth. In this paper, we discuss the development of an artificial neural network-based model to study the precursor leading to intense and moderate geomagnetic storms, following halo coronal mass ejection (CME) and related interplanetary (IP) events. IP inputs were considered within a 5-day time window after the commencement of storm. The artificial neural network (ANN) model training, testing and validation datasets were constructed based on 110 halo CMEs (both full and partial halo and their properties) observed during the ascending phase of the 24th solar cycle between 2009 and 2014. The geomagnetic storm occurrence rate from halo CMEs is estimated at a probability of 79%, by this model.     

Effects of coronal mass ejections on distant coronal streamers

The effects of a large coronal mass ejection (CME) on a solar coronal streamer located roughly 90° from the main direction of the CME propagation observed on January 2, 2012 by the SOHO/LASCO coronograph are analyzed. Radial coronal streamers undergo some bending when CMEs pass through the corona, even at large angular distances from the streamers. The phenomenon resembles a bending wave traveling along the streamer. Some researchers interpret these phenomena as the effects of traveling shocks generated by rapid CMEs, while others suggest they are waves excited inside the streamers by external impacts. The analysis presented here did not find convincing arguments in favor of either of these interpretations. It is concluded that the streamer behavior results from the effect of the magnetic field of a moving magnetic flux rope associated with the coronal ejection. The motion of the large-scale magnetic flux rope away from the Sun changes the surrounding magnetic field lines in the corona, and these changes resemble the half-period of a wave running along the streamer.     

Large-scale activity in solar eruptive events of October–November 2003 observed from SOHO/EIT data

Large-scale solar disturbances associated with powerful flares and coronal mass ejections (CMEs) during two passages of a grand system of three active regions in October–November 2003 are analyzed using data obtained with the SOHO/EIT EUV telescope. Dimmings (transient coronal holes) and, to a lesser extent, coronal waves (traveling emitting fronts) are studied using fixed-difference derotated images, in which a correction for the solar rotation is applied and a single heliogram preceding the event is subtracted from all subsequent heliograms. This method allows us to study difference heliograms in both the 195 Å line (with an interval of 12 min) and the various-temperature channels of 171, 195, 284, and 304 Å (with an interval of six hours). Our analysis shows, in particular, that the disturbances associated with CMEs demonstrated a global character and occupied almost the entire southern half of the disk in virtually all eruptive events during the two solar rotations. At the same time, the northern half of the disk, which had a large coronal hole, was only slightly disturbed. The dominant dimmings were observed on the disk as narrow, long features stretched mainly between three main, well-separated regions of the system and as long structures located along lines of solar latitude in the south polar sector. For repetitive events with intervals between them being not so long, the dominant dimmings demonstrated a clear homology in their forms and locations. During the very powerful event of October 28, one homologous global set of dimmings changed to another set. Many dimmings were observed to be identical or very similar in the three coronal channels and the transition-region line. It follows from the analysis that rapidly recovering global structures in the corona and transition region were involved in the eruption of running CMEs and the corresponding reconstruction of the large-scale magnetic fields.     

The role of plasma ejections in the development of large solar flares of various durations

Recent observations indicate that relatively strong plasma ejections are accompanied by the formation of systems of coronal loops with two glowing ribbons near their footpoints. However, while two-ribbon flares can sometimes last for many hours, for example, soft X rays, they sometimes decay within tens of minutes. We study here factors affecting the durations of flares using four major flares occurring in July 15–18, 2002, as examples. Various ground-based and satellite observations are used to show that short-duration events involved collimated (narrow) plasma ejections directed to the north and the subsequent formation of compact loops in the leading part of the active region. During one event, a powerful eastward ejection in a wide solid angle was followed by the formation of an extended arch system in the trailing part, which determined the long duration of the flare. It is proposed that in events involving collimated jets and corresponding narrow features in coronal mass ejections (CMEs), systems of coronal loops do form, but post-eruptive energy release either does not occur or is expressed very faintly. So the energy does not go downward from this region, and the plasma is emitted free in the coronal loops. In contrast to such rapid flares, wide ejections and bright, large-scale CMEs are accompanied by the formation and prolonged existence of an extended arch system. Thus, powerful nonstationary solar processes involve a large-scale CME and the flare itself, with the pattern of a particular event determined by the reconnection scenario and the evolution of the ejected plasma.     

Solar large-scale channeled dimmings produced by coronal mass ejections

A new type of dimmings, or transient coronal holes (i.e., regions of reduced soft-X-ray and EUV emission), is revealed in analyses of difference solar images obtained with the SOHO EIT ultraviolet telescope at 195 Å. Such features can be observed on the solar disk after halo-type coronal mass ejections (CMEs). If several active regions, filaments, and other structures are present on the disk during a major eruptive event, then strongly anisotropic, channel-shaped (“channeled”) dimmings coexist with relatively compact dimmings adjacent to the eruption center. The channeled dimmings are comparable to the compact dimmings in terms of their contrast; stretch along several narrow, extended features (channels); and can span nearly the entire visible disk. Coronal waves, which appear as fronts of enhanced brightness traveling ahead of the dimmings in some halo CME events, are also anisotropic. We argue that such transient phenomena are closely related to the strong disturbance and restructuring of large-scale magnetic fields involved in CMEs, and the channeled character of the dimmings reflects the complexity of the global solar magnetosphere, in particular, near the solar-activity maximum.     

Form of the latitude distribution of sunspot activity

The spatial (latitude) distribution of sunspots is studied, including its dependence on solar activity. It is shown that the latitude distributions of sunspots for a given year can be approximately described by the normal law, with its variance being a linear function of the current level of solar activity. Thus, an increase in activity is accompanied by an expansion of the zone of solar activity, in good agreement with earlier results. As the solar activity increases, the width of the zone of sunspot generation and the latitude maximum of the sunspot density grow somewhat more slowly than the number of sunspots, in agreement with observations. The results obtained can be used to reconstruct the spatial distributions of sunspots in the past, interpret the magnetic activity of stars, and address the requirements of the dynamo theory in the form of constraints imposed on models of cyclicity.     

Large-scale activity in major solar eruptive events of November 2004 according to SOHO data

Data obtained with the EIT UV telescope and LASCO coronagraph of the SOHO satellite are used to analyze large-scale solar disturbances associated with a series of major flares and coronal mass ejections that occurred in the late decline phase of cycle 23, on November 3–10, 2004, and gave rise to strong geomagnetic storms. Derotated fixed-base difference heliograms taken in the 195 Å coronal channel at 12-min intervals and in the various-temperature 171, 195, 284, and 304 Å channels at 6-h intervals indicate that these disturbances were global and homologous; i.e., they had similar characteristics and affected the same structures. Almost all of the nine events of this series included two recurrent systems of large-scale dimmings (regions of reduced intensity with lifetimes of 10–15 h): (a) transequatorial dimmings connecting a northern near-equatorial eruption center with a southern active region and (b) northern dimmings covering a large sector between two coronal holes. In this northern sector, coronal waves (brightenings propagated from the eruption center at speeds of several hundred km/s) were observed ahead of the expanding dimmings. The brightest, central part of the halo-type coronal mass ejection in each event corresponded to the northern dimming system. The properties of the dimmings and coronal waves and the relationship between them are discussed on the basis of the results obtained. We find that the eruption of large coronal mass ejections involves structures of the global solar magnetosphere with spatial scales far exceeding the sizes of active regions and normal activity complexes.     

Some features of the streamer belt in the solar corona and at the Earth’s orbit

The rays of enhanced brightness making up the structure of the coronal-streamer belt can be traced to the lowest atmospheric layers in the Sun, with the angular size remaining nearly constant, d ≈ 2.5° ± 0.5°. This suggests that the physical mechanism generating the slow solar wind in the rays of the streamer belt differs from the mechanism giving rise to the fast solar wind from coronal holes. At distances of R < (4–5) R _⊙, the rays of the streamer belt are not radial in the plane of the sky and show deviations toward the corresponding pole. They then become essentially radial at R > (4–5) R _⊙. A transverse cross section of streamers in the corona and its continuation into the heliosphere—a plasma sheet—can be represented as two radially oriented, closely spaced rays (d ≈ 2.0°–2.5°) with enhanced density and an angular size of d. We also show that the ray structure of the streamer belt is involved in the development of coronal mass ejections (CMEs). The motion of a small-scale CME occurs within a magnetic flux tube (ray of enhanced brightness) and leads to an explosive increase in its angular size (rapid expansion of the tube). It seems likely that large-scale CMEs are the result of the simultaneous expansion of several magnetic tubes. We suggest that a small-scale CME corresponds to a “plasmoid” (clump of plasma of limited size with its own magnetic field) ejected into the base of a magnetic tube, which subsequently moves away from the Sun along the tube.     

On the correlation between spectra of solar microwave bursts and proton fluxes near the Earth

Studies of the extreme solar proton event of January 20, 2005 intensified the contest over of a long-standing problem: are solar cosmic rays arriving at the Earth accelerated by solar flares or by shocks preceding rapidly moving coronal mass ejections? Among the most important questions is the relationship between the energy spectra of the solar cosmic rays and the frequency spectra of flare microwave bursts. Some studies of previous solar-activity cycles have shown that such a relationship does exist, in particular, for protons with energies of tens of MeV. The present work analyzes this relation using data for 1987–2008. For flare events observed in the western half of the disk, there is a significant correlation between the index δ, which is equivalent to the power-law index of the integrated energy spectrum of 10–100 MeV protons detected near the Earth’s orbit, and radio burst parameters such as a ratio of peak fluxes S at two frequencies (for example, at 9 and 15 GHz) and a microwave peak frequency f _m . Proton fluxes with hard (flat) energy spectra (δ ≤ 1.5) correspond to hard microwave frequency spectra (S ₉/S ₁₅ ≤ 1 and f _m ≥ 15 GHz), while flares with soft radio spectra (S ₉/S ₁₅ ≥ 1.5 and f _m ≤ 5 GHz) result in proton fluxes with soft (steep) energy spectra (δ ≥ 1.5–2). It is also shown that powerful high-frequency bursts with the hardest radio spectra (f _m ≈ 30 GHz) can point at acceleration of significant proton fluxes in flares occurring in strong magnetic fields. These results argue that solar cosmic rays (or at least their initial impulses) are mainly accelerated in flares associated with impulsive and post-eruptive energy release, rather than in shocks driven by coronal mass ejections.