敦德冰芯过去800a来的甲烷记录

郭德冰芯上部９５ｍ的１２个样品记录了近８００ａ来冰内气泡包裹气体中甲烷的浓度变化,结果表明,最近２００ａ来该冰芯记录的甲烷浓度急剧上升,与南极及格陵兰的甲烷记录反映的趋势相一致,但与两极同时代样品相比,其浓度总体上要高出０．５×１０＾－６～０．６×１０＾－６ｍｏｌ／ｍｏｌ在这之前,３者基本保持一致,在０．７×１０＾－６～０．８×１０＾－６ｍｏｌ／ｍｏｌ之间波动。     

Concerning the generation of geomagnetic giant pulsations by drift-bounce resonance ring current instabilities

Giant pulsations are nearly monochromatic ULF-pulsations of the Earth’s magnetic field with periods of about 100 s and amplitudes of up to 40 nT. For one such event ground-magnetic observations as well as simultaneous GEOS-2 magnetic and electric field data and proton flux measurements made in the geostationary orbit have been analysed. The observations of the electromagnetic field indicate the excitation of an odd-mode type fundamental field line oscillation. A clear correlation between variations of the proton flux in the energy range 30–90 keV with the giant pulsation event observed at the ground is found. Furthermore, the proton phase space density exhibits a bump-on-the-tail signature at about 60 keV. Assuming a drift-bounce resonance instability as a possible generation mechanism, the azimuthal wave number of the pulsation wave field may be determined using a generalized resonance condition. The value determined in this way, m = −21±4, is in accord with the value m = −27±6 determined from ground-magnetic measurements. A more detailed examination of the observed ring current plasma distribution function f shows that odd-mode type eigenoscillations are expected for the case ∂f/∂W ≥ 0, much as observed. This result is different from previous theoretical studies as we not only consider local gradients of the distribution function in real space, but also in velocity space. It is therefore concluded that the observed giant pulsation is the result of a drift-bounce resonance instability of the ring current plasma coupling to an odd-mode fundamental standing wave. The generation of the bump-on-the-tail distribution causing ≥f/≥W ≥ 0 can be explained due to velocity dispersion of protons injected into the ring current. Both this velocity dispersion and the necessary substorm activity causing the injection of protons into the nightside magnetosphere are observed.     

Spectral characteristics of waves and particles in the model of cyclotron wave-particle interactions near plasmapause

Further analysis of energetic electron precipitation at the evening sector of magnetosphere is performed. In the framework of the quantitative model of cyclotron wave-particle interactions developed in the previous Pasmanik et al. paper, the case of finite spread over energies of initial energetic electron distribution is studied. The solution for distribution function of energetic electron is found. The energetic spectrum of trapped and precipitating electrons and whistler wave spectrum are analysed.     

Resonant enhancement of relativistic electron fluxes during geomagnetically active periods

The strong increase in the flux of relativistic electrons during the recovery phase of magnetic storms and during other active periods is investigated with the help of Hamiltonian formalism and simulations of test electrons which interact with whistler waves. The intensity of the whistler waves is enhanced significantly due to injection of 10–100 keV electrons during the substorm. Electrons which drift in the gradient and curvature of the magnetic field generate the rising tones of VLF whistler chorus. The seed population of relativistic electrons which bounce along the inhomogeneous magnetic field, interacts resonantly with the whistler waves. Whistler wave propagating obliquely to the magnetic field can interact with energetic electrons through Landau, cyclotron, and higher harmonic resonant interactions when the Doppler-shifted wave frequency equals any (positive or negative) integer multiple of the local relativistic gyrofrequency. Because the gyroradius of a relativistic electron may be the order of or greater than the perpendicular wavelength, numerous cyclotron, harmonics can contribute to the resonant interaction which breaks down the adiabatic invariant. A similar process diffuses the pitch angle leading to electron precipitation. The irreversible changes in the adiabatic invariant depend on the relative phase between the wave and the electron, and successive resonant interactions result in electrons undergoing a random walk in energy and pitch angle. This resonant process may contribute to the 10–100 fold increase of the relativistic electron flux in the outer radiation belt, and constitute an interesting relation between substorm-generated waves and enhancements in fluxes of relativistic electrons during geomagnetic storms and other active periods.     

Effects of a sloping thermocline and Rayleigh friction on equatorially trapped Kelvin waves

INTRODUCTIONEquatorialKelvinwavesareofspecialsignificanceinthedynamicsoftheequatorialocean ,duetotheirhighpropagationspeedandequatoriallytrappednature.NumericalandobservationalstudiesstronglysuggestedthatKelvinwavesplayamajorroleinElNi no SouthernOscillationandotheroceanphenomena.Themainthermoclinevariabilityinthetropicaloceanswasstudiedextensivelybyvariousre searchers (LongandChang ,1 990 ;YangandYu ,1 992 ) .Animportantfeatureoftheequatorialoceanthermalstructureistheeastwardshoaling…     

昆仑山断裂带围陷波的有限差分数值模拟解释

利用交错网格有限差分方法对昆仑山断裂带人工爆破产生的围陷波进行了三维数值模拟解释.为提高断裂带最终模型的可信度,在围陷波模拟的同时考虑了人工爆破记录的三个分量.对昆仑山断裂带围陷波的模拟结果表明,影响围陷波特性的断裂带深度主要在10 km以内.S波速度和断裂带宽度对围陷波的到时、频率、振幅和相位影响较大.数值模拟解释获得的昆仑山断裂带的细结构参数是：浅部断裂带宽度为300 m,深部为250 m;深度在400 m以上断裂带内S波速度为098 km/s,外部围岩S波速度为170 km/s,Q值为138;S波速度和Q值随着深度的增加而增加;1000 m以下断裂带内S波速度为280 km/s,围岩S波速度为33 km/s.     

Measurement of the secular motion frequency and the space charge density in the linear ion trap

This paper reports that a cloud of laser-cooled ⁴⁰Ca⁺ is successfully trapped and manipulated in the home-built linear ion trap constructed for quantum information processing (QIP). The frequency of the secular motion and the space charge density of the ion cloud are measured, which help knowing the characteristic of the trapping potential and are the prerequisite of QIP with the trapped ions.     

海啸俘获波在弯曲海脊上的传播规律

越洋海啸会受大洋海脊的引导以俘获波的形式沿其传播上万千米,其携带的巨大能量会严重影响远场地区、威胁海岸地区的安全。本文基于MIKE21-BW模型,分别模拟0°(直海脊)至90°(直角弯曲海脊)不同弯曲角度海脊上俘获波的传播变形过程,并定量比较其能量分配。结果表明,海脊俘获波传至海脊转弯处,少部分能量会泄露出海脊重新以自由波的形式扩散至整个海域;部分能量会被反射回来形成与初始海啸波相反方向的俘获波沿海脊传播,反射的能量会随着海脊弯曲角度的增加而增加;还有一部分能量继续沿着弯曲的海脊向前传播,其随着海脊弯曲的角度增加而减小。     

基于射线理论的海脊俘获波机制

虽然众多现场实测资料和数值模拟均表明海脊可以俘获海啸波并引导其传播至远场地区,带来严重的灾害,但少有研究阐述其产生机理。本文基于射线理论,推导了指数型海脊上波浪传播轨迹的理论解,并提出了震源位于海脊顶部的海啸被海脊完全俘获的条件。基于该俘获条件进一步给出了海脊对海啸俘获效率的表达式,用以评估海啸中被海脊俘获影响至远场的能量占海啸总能量的比例。     

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