月壤中的稀有气体

月球极度亏损挥发分,但是月壤中赋存有大量的稀有气体,主要来源于太阳风注入、宇宙射线作用和放射性同位素衰变等过程。月岩和月壤样品的稀有气体研究,不仅是获取月球表面形成和演化历史、近地空间小行星撞击历史等的重要内容,更是解译40亿年以来太阳风演化的惟一可行途径。本文主要介绍月岩和月壤中的太阳风记录、宇宙射线暴露年龄、Ar-Ar定年以及稀有气体测试技术等方面研究的进展。     

Heinrich事件和末次冰期气候的不稳定性

对北大西洋深海沉积物的研究表明：末次冰期北大西洋沉积物记录中有多次洋面温度降低、有孔虫含量减少、盐度降低和粗颗粒的碳酸盐碎屑快速堆积的现象，这些时间跨度上千年或几百年的气候快速波动被称为Heinrich事件^{［１－４］}，很难用古气候的米兰科维奇理论来解释。最近对末次冰期中国马兰黄土堆积的调查发现，在末次冰期之中东亚冬季风也有多次加强，它与北大西洋沉积物中的Heinrich事件对应很好，暗示着东亚季风的变迁更直接受控于北半球冰量的变化，而不是过去人们认为的东亚古季风气候变化与地球轨道变化引起太阳辐射变化直接相关。      

Apollo 11月壤样品中太阳风成因的水及其意义

为研究太阳风成因水在月表低纬度地区的分布特征,本文对中国科学院地质与地球物理研究所博物馆珍藏的一份Apollo 11月壤样品开展了单颗粒原位纳米离子探针H同位素和水含量深度剖面分析。结果表明月壤颗粒表层(<200nm)具有较高的水含量(剖面最大水含量变化范围为0.35%～1.59%,平均值为0.82%),该结果与前人对Apollo样品的报导类似。除一颗斜长石的H同位素组成(δD=-262‰)落在月幔范围内,其余颗粒表层均非常贫D(δD变化范围为-987‰～-642‰)。该强烈贫D的同位素组成与太阳风一致,完全不同于地球大气水,不仅证明这些样品的月球来源,并且主要是太阳风注入的贡献。矿物颗粒之间的水含量和δD值变化,很可能与太阳风注入后的扩散丢失程度不同有关。另外,我们观察到橄榄石、单斜辉石和长石的水含量剖面比较类似,整体呈现随深度逐渐递减的趋势。相比之下,玻璃质颗粒的水含量剖面呈现随深度先上升再降低的峰形特征,峰位在25～43nm深度。这两者之间的差异很可能跟H在矿物和玻璃中的扩散速率、辐射损伤层等的差异有关。本项研究也证明,即使对于H这样易于受地球污染的元素,在普通条件下(北京...     

北太平洋Rossby波研究进展

系统地阐述了北太平洋Rossby波在卫星观测、理论扩展及模型应用3个方面的研究成果.随着卫星观测技术的发展,明显地探测到海表面信号的Rossby波特征,且观测到波速在热带外大于自由Rossby波理论值.为解释这个波动加速现象,在自由Rossby渡理论的基础上,考虑了大气强迫、非静止基流及海底地形等因子的作用,使得Rossby波的波动理论得到了扩展.而关于风应力强迫Rossby波的线性理论模型主要有3类:一阶斜压Rossby波模型、局地Ekman抽吸模型和Svetdrup平衡模型.这些模型被广泛地应用到北太平洋海表面高度和温度/密度跃层深度等要素变化的机理研究中,得到了不同的模型在大洋的不同区域有不同的作用等结论.最后,对线性Rossby波研究存在的问题进行了初步探讨,提出了需要进一步解决的新课题.     

瞬变电磁测深中数据处理偏差及修正方法

瞬变电磁测深方法中通常采用阶跃波激励方式的模型进行处理。在实际应用中,为了便于重复观测,一般采用方波形式进行激励,采用阶跃波模型进行数据处理和解释;这种处理方式理论上存在比较大的偏差。为了修正这种偏差,通过理论计算,建议采用单脉冲电磁测深方法来处理方波激励源的电磁测深结果。实例分析表明,该方法是可行的。     

西藏波龙斑岩铜金矿床钾长石和绢云母40Ar/39Ar年龄及其地质意义

西藏波龙斑岩铜金矿床是新近在青藏高原中部发现的规模最大的斑岩型矿床。文章对该矿床内的蚀变钾长石和蚀变绢云母进行了⁴⁰Ar/³⁹Ar年代学测试,获得蚀变钾长石的⁴⁰Ar/³⁹Ar坪年龄为(118.33±0.60) Ma,反等时线年龄为(118.49±0.74) Ma (初始⁴⁰Ar/³⁶Ar=286.1±8.4),表明波龙斑岩铜金矿床的钾化蚀变年龄为118~119 Ma;蚀变绢云母的⁴⁰Ar/³⁹Ar坪年龄为(121.61±0.67) Ma,反等时线年龄为(121.1±2.0) Ma (初始⁴⁰Ar/³⁶Ar=279±19)。由于蚀变绢云母测试样品内可能混入了斜长石,受其影响,蚀变绢云母测年结果的下限可能代表了该矿床绢英岩化蚀变年龄。这些蚀变钾长石和蚀变绢云母⁴⁰Ar/³⁹Ar测年结果与波龙矿床的成岩年龄值和成矿年龄值在误差范围内基本一致,表明该矿床的钾化和绢英岩化与成岩、成矿同期,该矿床的岩浆-热液活动过程的时限为121~118 Ma。     

高Rb/Sr岩石样品中Sr同位素多接收等离子体质谱分析校正方法研究

在利用多接收电感耦合等离子体质谱(MC-ICPMS)进行Sr同位素研究中,⁸⁷Rb对于⁸⁷Sr干扰严重。岩石样品经化学分离后,若Rb/Sr≤0.0005,可以采用传统的Rb干扰扣除方法对⁸⁷Sr/⁸⁶Sr测定值进行准确校正;但如果样品经化学分离后仍含有较高的Rb/Sr比,同量异位素的干扰不能完全消除,则无法准确校正⁸⁷Sr/⁸⁶Sr测定值,直接影响测试结果的准确度。本文针对Rb含量较高的地质样品设计两组实验,确定了⁸⁷Sr/⁸⁶Sr同位素比值与Rb/Sr元素含量比值的关系曲线,并在理论分析的基础上,提出包含同位素分馏校正在内的重叠干扰校正方法。通过实际地质样品验证,该校正方法在较高含量Rb元素共存(Rb/Sr<0.2)的Sr纯化液中,能够较为准确地测量⁸⁷Sr/⁸⁶Sr同位素比值,降低了MC-ICPMS分析地质样品中Sr同位素时对化学分离步骤的要求。而对于Rb/Sr>0.2的地质样品,因仪器分馏效应和记忆效应影响,测试精确度大大降低,无论采用何种校正方法均无法得到准确的Sr同位素组成。     

地球液核的动力学效应研究进展

简要介绍了液核动力学研究的方法及液核动力学效应检测的进展和研究结果,着重介绍了超导重力仪在液核动力学研究中的作用。基于初始参考地球模型（PREM）,采用球对称、非自转、完全弹性和各向同性地球的弹性引力形变理论研究了液核动力学扰动导致的地球固体部分的形变和重力位扰动。根据重力潮汐观测中的近周日共振特征,利用国际超导重力仪观测资料研究了地球的自由核章动（FCN）,精密确定了有关的共振参数,其中FCN的本征周期为429.0（424.3,4 433.7）恒星日,品质因子为 9543（6405,18714）,复共振强度为（－6.10±0.20,－0.01±0.20）×10^－4°/h。最近,我们还估计了全球地球动力学观测网中全球分布的14台超导重力仪21个长期、连续重力观测序列的"积谱密度"以检测固体内核的平动振荡运动。     

低δ18O岩浆岩的成因

具有显著低于正常幔源岩浆δ¹⁸O值的岩浆岩是地球上比较罕见的一种岩石,其形成需要特殊的岩浆过程。虽然岩浆分异过程基本上不改变氧同位素组成,但水岩反应可以明显改变岩石的氧同位素组成,高温水岩反应会导致岩石的氧同位素组成显著降低,这得到了理论计算的支持。对黄石高原流纹岩和冰岛玄武岩这两个典型的低δ¹⁸O岩浆实例的长期研究发现, 在地表遭受了高温热液蚀变的低δ¹⁸O岩石部分熔融或者被岩浆同化是形成低δ¹⁸O岩浆的重要机制,这通常通过裂谷构造带破火山口的垮塌来实现。塞舌尔和碾子山代表了结晶于低δ¹⁸O岩浆的花岗岩实例,其形成需要源区有亏损¹⁸O的地壳物质参与。大别-苏鲁造山带超高压变质岩亏损¹⁸O的幅度和这些亏损¹⁸O岩石的分布面积都非常令人瞩目。对这些超高压变质岩的原岩进行氧同位素研究,能够为其这些低δ¹⁸O岩石的成因提供有力的制约。目前已经在北淮阳花岗岩中报道了具有新元古代年龄和低δ¹⁸O 值的锆石。研究显示,这些花岗岩可能经历了两次高温水岩反应,第一次导致了低¹⁸O岩浆的形成和低δ¹⁸O值锆石的结晶,第二次则进一步降低了其它矿物的δ¹⁸O值,导致了氧同位素不平衡。对这些低δ¹⁸O花岗岩的深入研究,特别是进行原位微区分析,不仅有助于我们深入认识低δ¹⁸O岩浆的形成机理,而且有助于进一步理解水岩反应中元素和同位素的地球化学行为。     

空间物理学的回顾和展望

空间物理学是一门重要的迅速发展的学科。回顾了过去百年中发生的重大空间物理学事件。空间物理学已成功地迈过了探索阶段 ,未来是要搞清一些基本的科学问题。这些问题的解决需要观测研究、理论分析、数值模拟和环境预报的紧密合作 ,才能促成空间物理学的飞跃发展。     

Do lunar and meteoritic archives record temporal variations in the composition of solar wind noble gases and nitrogen? A reassessment in the light of Genesis data

Since about half a century samples from the lunar and asteroidal regoliths been used to derive information about elemental and isotopic composition and other properties of the present and past solar wind, predominantly for the noble gases and nitrogen. Secular changes of several important compositional parameters in the solar wind were proposed, as was a likely secular decrease of the solar wind flux. In 2004 NASA’s Genesis mission returned samples which had been exposed to the solar wind for almost 2.5 years. Their analyses resulted in an unprecendented accuracy for the isotopic and elemental composition of several elements in the solar wind, including noble gases, O and N. The Genesis data therefore also allow to re-evaluate the lunar and meteorite data, which is done here. In particular, claims for long-term changes of solar wind composition are reviewed.Outermost grain layers from relatively recently irradiated lunar regolith samples conserve the true isotopic ratios of implanted solar wind species. This conclusion had been made before Genesis based on the agreement of He and Ne isotopic data measured in the aluminum foils exposed to the solar wind on the Moon during the Apollo missions with data obtained in the first gas release fractions of stepwise in-vacuo etch experiments. Genesis data allowed to strengthen this conclusion and to extend it to all five noble gases. Minor variations in the isotopic compositions of implanted solar noble gases between relatively recently irradiated samples (<100 Ma) and samples irradiated billions of years ago are very likely the result of isotopic fractionation processes that happened after trapping of the gases rather than indicative of true secular changes in the solar wind composition. This is particularly important for the ³He/⁴He ratio, whose constancy over billions of years indicates that hardly any ³He produced as transient product of the pp-chains has been mixed from the solar interior into its outer convective zone. The He isotopic composition measured in the present-day solar wind therefore is identical to the (D + ³He)/⁴He ratio at the start of the suns’s main sequence phase and hence can be used to determine the protosolar D/H ratio.Genesis settled the long-standing controversy on the isotopic composition of nitrogen in lunar regolith samples. The ¹⁵N/¹⁴N ratio in the solar wind as measured by Genesis is lower than in any lunar sample. This proves that nitrogen in regolith samples is dominated by non-solar sources. A postulated secular increase of ¹⁵N/¹⁴N by some 30% over the past few Ga is not tenable any longer. Genesis also provided accurate data on the isotopic composition of oxygen in the solar wind, invaluable for cosmochemisty. These data superseded but essentially confirmed one value – and disproved a second one – derived from lunar regolith samples shortly prior to Genesis.Genesis also confirmed prior conclusions that lunar regolith samples essentially conserve the true elemental ratios of the heavy noble gases in the solar wind (Ar/Kr, Kr/Xe). Several secular changes of elemental abundances of noble gases in the solar wind had been proposed based on lunar and meteoritic data. I argue here that lunar data – in concert with Genesis – provide convincing evidence only for a long-term decrease of the Kr/Xe ratio by almost a factor of two over the past several Ga. It appears that the enhancement of abundances of elements with a low first ionisation potential in the solar wind (FIP effect) changed with time.Finally, Genesis allows a somewhat improved comparison of the present-day flux of solar wind Kr and Xe with the total amount of heavy solar wind noble gases in the lunar regolith. It remains unclear whether the past solar wind flux has been several times higher on average than it is today.     

The outer scale of solar-wind turbulence from GALILEO coronal-sounding data

Radio sounding experiments on of the solar plasma were carried out by the GALILEO spacecraft using S-band (2295 MHz) signals in 1995–1996 a period of minimum solar activity. Equatorial regions at heliocentric distances of 7–80 solar radii were studied. The frequency of the received signal was detected by three ground stations. By carrying out continuous observations of unprecedented duration and processing the data using spectral and correlation methods, we have obtained reliable information on large-scale inhomogeneities of the solar-wind density for the first time. The outer turbulence scale increases with heliocentric distance, the dependence being close to linear. We estimate the outer turbulence scale and analyze its dependence on distance from the Sun and local plasma parameters for a model in which the outer scale is formed due to competition between the linear amplification of Alfven waves in the irregular, moving solar-wind plasma and the nonlinear transfer of turbulent energy to higher frequencies. A comparison of predictions for various specific cases of this model with the observational data suggests that the main nonlinear processes responsible for the formation of the inertial range of the spectrum on the investigated scales are three-wave decay processes involving Alfven and magnetoacoustic waves.     

Long and short term relationships between solar wind velocity and geomagnetic field at low latitudes

Solar wind velocity control of low latitude geomagnetic field both on long and short term basis is studied. It is shown that semiannual averages of the low latitude field is inversely related to solar wind velocity and that there is a dominant local time dependence of the relationship. Strongest correlation are confined to the local afternoon hours. It is also shown that for a duration when the solar wind velocity exhibits significant recurrent pattern the low latitude geomagnetic field also depicts strong solar synodic rotation periodicity of 27 days with significant coherence with velocity. The low latitude field on a short term basis is influenced by variable solar wind velocity with a delay of about 1–2 days. During the period of systematic recurrent pattern in solar wind velocity even the quiet-time night field at equatorial and low latitudes show a strong dependence on velocity indicative of the solar wind control of the quiet-time proton belt encompassing the earth.     

Spatial distribution of turbulence characteristics in the inner solar wind

Data on the spatial distributions of turbulence characteristics in the inner solar wind are reported. Spectral indices for the outer and inner turbulence scales have been obtained in radio occultation experiments using signals from several spacecraft at different phases of the solar cycle. The characteristics of turbulence in the slow, low-latitude solar wind remain, on average, constant during the solar cycle. The outer turbulence scale in the fast, high-latitude solar wind appreciably exceeds that of the slow, low-latitude wind at the solar minimum. The new data confirm that the transition from the acceleration region to the steady-flow region is accompanied by a change in the turbulence regime. This change in the turbulence regime takes place at greater distances from the Sun for the fast than for the slow solar wind.     

Observations of the atmospheric surface layer parameters over a semi arid region during the solar eclipse of August 11th, 1999

This paper discusses the observations of the Atmospheric Surface Layer (ASL) parameters during the solar eclipse of August 11th, 1999. Intensive surface layer experiments were conducted at Ahmedabad (23‡21′N, 72‡36′E), the western part of India, which was close to the totality path. This rare event provided by nature is utilised to document the surface layer effects during the eclipse period using measurements of high frequency fluctuations of temperature, tri-axial wind components as well as mean parameters such as temperature, humidity, wind speed and subsoil temperature. Analysis showed that during the eclipse period, the turbulence parameters were affected leading to the suppression of the turbulence process, the main dynamic process in the atmospheric boundary layer, while the mean parameters showed variations within the natural variability of the observational period. The spectra of the wind components and temperature indicated decrease in spectral power by one order in magnitude during the eclipse period. The rate of dissipation of turbulent kinetic energy is found to decrease by more than one order during the eclipse period. The stability parameter showed a change from unstable to stable condition during the period of eclipse and back to unstable condition by the end of eclipse     

On Possible Types of Magnetospheres of Hot Jupiters

As a rule, the orbits of “hot Jupiter” exoplanets are located close to the Alfven point of the stellar wind of the host star. Many hot Jupiters could be in the sub-Alfven zone, where the magnetic pressure of the stellar wind exceeds the dynamical pressure. Therefore, the magnetic field in the wind should play an extremely important role in the process of stellar wind flowing around the atmosphere of a hot Jupiter. This must be taken into account when constructing theoretical models and interpreting observational data. Analyses show that many typical hot Jupiters should have shockless induced magnetospheres, which have no analogs in the solar system. Such magnetospheres are characterized first and foremost by the fact that there is no bow shock, and the magnetic barrier (ionopause) is formed by induced currents in upper layers of the ionosphere. This conclusion is confirmed here using three-dimensional numerical simulations of the flow of the stellar wind from the host star around the hot Jupiter HD 209458b, taking into account both the intrinsic magnetic field of the planet and the magnetic field in the wind.

     

Solar Wind Magnetic Field Turbulence over the Solar Activity Cycle Inferred from Coronal Sounding Experiments with Helios Linear-Polarized Signals

Results of experiments on polarized radio sounding of the outer solar corona using the Helios spacecraft from 1975 to 1984 are presented. The characteristic parameters of the temporal spectra of fluctuations in the Faraday rotation of the plane of polarization for heliocentric distances from 3.5 to 5.5 solar radii are obtained. The absolute level of these fluctuations and, consequently, the level of fluctuations of the magnetic field, is almost independent of the solar activity. It is well known that the global structure of the solar wind varies with the solar cycle such that there is slow solar wind at low latitudes and fast solar wind at high latitudes during solar minima. In contrast, a slow solar wind dominates at all latitudes during solar maxima. One explanation for the invariance of the fluctuations observed by sounding the circumsolar plasma is that the mean magnetohydrodynamic turbulence of the low-latitude, slow solar wind depends weakly on the phase of the solar cycle.

     

Origins and properties of the quasi-stationary slow solar wind

Comparisons of the brightness distributions of the white corona observed at distances of several solar radii with solar wind velocities derived from interplanetary-scintillation observations, as well as analyses of solar wind data obtained on spacecraft from December 1994 to June 1995, indicate that the fast solar wind can contain plasma with velocities V ≈ 300–450 km/s, approaching those typical for the slow solar wind that flows in the streamer belt and chains of streamers. At the same time, certain other parameters, first and foremost the plasma density N and ratio T/N ^0.5 (where T is the temperature), indicate that these two flows differ considerably. The slow solar wind flowing in the streamer belt and chains displays high densities N > 10 ± 2 cm^?3 and low T/N ^0.5 < 1.7 × 10⁴ K cm^3/2 at the Earth’s orbit. The number of slow solar-wind sources observed in chains can be comparable with the number observed in the belt. The fast solar wind flowing from coronal holes always displays low densities N≤ 8 cm^?3 and high T/N ^0.5 > 1.7 × 10⁴ K cm^3/2. These properties probably indicate different origins of the fast and slow solar winds.     

Turbulence in the inner solar wind determined from frequency fluctuations of the downlink signals from the ULYSSES and GALILEO spacecraft

The results of several sets of measurements of the frequency of radio signals during coronal-sounding experiments carried out from 1991 to 2000 using the ULYSSES and GALILEO spacecraft are presented and analyzed. The S-band signals (carrier frequency f = 2295 MHz) were received at the three 70-m widely spaced ground stations of the NASA Deep Space Network. As a rule, the frequency-fluctuation spectra at frequencies above 1 mHz are power-laws. At small heliocentric distances, R < 10R_⊙ (R_⊙ is the solar radius), the spectral index is close to zero; this corresponds to a spectral index for the one-dimensional turbulence spectrum p₁ = 1. The index of the frequency-fluctuation spectra in the region of the supersonic solar wind at distances R > 30 R_⊙ is between 0.5 and 0.7 (p₁ = 1.5–1.7). The results demonstrate a substantial difference between the turbulence regimes in these regions: in the region of the established solar wind, the power-law spectra are determined by nonlinear cascade processes that pump energy from the outer turbulence scale to the small-scale part of the spectrum, whereas such cascade processes are absent in the solar wind acceleration region. Near the solar minimum, the change in the turbulence regime of the fast, high-latitude solar wind occurs at greater distances than for the slow, low-latitude solar wind. Spectra with a sharp cutoff at high frequencies have been detected for the first time. Such spectra are observed only at R < 10 R_⊙ and at sufficiently low levels of the electron density fluctuations. The measured cutoff frequencies are between 10 and 30 mHz; the cutoff frequency tends to increase with heliocentric distance. The variance of the plasma-density fluctuations has been estimated for the slow, low-latitude solar wind. These estimates suggest that the relative fluctuation level at distances 7 R_⊙ < R < 30 R_⊙ does not depend on heliocentric distance. The cross correlation of the frequency fluctuations recorded at widely spaced ground stations increases with the index of the frequency-fluctuation spectrum. At distances R ≈ 10 R_⊙, the rate of temporal changes in irregularities on the scale of several thousand kilometers is less than or comparable to the solar wind velocity.     

Parameters of the turbulence of the interplanetary plasma derived from scintillation observations of the quasar 3C 48 at the solar-activity minimum

Temporal spectra of interplanetary scintillations of the strong radio source 3C 48 based on 111 MHz observations on the Large Scanning Antenna of the Lebedev Physical Institute obtained near the solar-activity minimum are analyzed. Measurements of the temporal spectrum of the scintillations are used to estimate the angular size of the source, the velocity of inhomogeneities, and the power-law index for the spatial spectrum of the turbulence in the interplanetary plasma. The mean angular size of the source is θ ₀ = 0.326″ ± 0.016″, and the mean index for the three-dimensional turbulence spectrum is n = 3.7 ± 0.2. There is some evidence that n decreases in the transition from the fast, high-speed to the slow, low-latitude solar wind.