临汾盆地晚冰期至中全新世黄土-古土壤序列的风化特征及指示的气候意义

了解中国北方晚冰期和全新世时期的气候环境变化及其驱动机制,有助于预测未来气候变化的可能情景。基于黄土高原东南缘临汾盆地的黄土-古土壤剖面,在3个AMS14C年代的支持下,通过粒度、磁化率、土壤有机碳以及地球化学元素等指标,重建了临汾盆地晚冰期至中全新世晚期的气候变化历史。结果表明：宋村沟剖面的黄土和古土壤分别处于初等和中等化学风化阶段,而不同地区风成堆积物的化学风化强度存在明显差异,主要受控于东亚夏季风的区域变化。多指标综合分析表明,晚冰期以来临汾盆地的气候演变经历了4个阶段：晚冰期东亚冬季风较强,气候干冷;早全新世东亚夏季风强化,气候向暖湿转变;早中全新世东亚夏季风达到峰值,为最暖湿的适宜期;中全新世晚期东亚夏季风减弱,气候再次转向干冷;临汾盆地的气候变化主要受控于北半球太阳辐射强度和冰量的变化。     

On measuring low-degree p-mode frequency splitting with full-disc integrated data

The standard method of measuring rotational splitting from solar full-disc oscillation data, based on maximum-likelihood fitting of multi-Lorentzian profiles to oscillation power spectra, systematically overestimates the splitting. One of the reasons is that the maximum likelihood estimators (MLE) become unbiased only asymptotically as the number of data tends to infinity; for a finite data set they are often biased, inducing a systematic error. In this paper we assess by Monte Carlo simulations the amount of systematic error in the splitting measurement, using artificially generated power spectra. The simulations are carried out for multiplets of degree     2 and 3 with various signal-to-noise ratios, linewidths and observing times. We address the possible use of non-MLE estimators that could provide a smaller or negligible systematic error. The implication for asteroseismology is also discussed.     

Pulsar radio emission

Radio emission by pulsars is calculated from first principles. In an almost current-free magnetosphere, the two charged components (of the unsteadily escaping pair plasma) have different (and varying) bulk Lorentz factors. Curvature radiation emitted by the more energetic component is thus locally coherent, (so-called antenna mechanism). Strong enough seed signals cause the relativistically streaming charges to enhance their radiation, via an induced drift that can largely exceed the curvature drift. This amplification mechanism is similar to - but different from - that of a maser; we call it a MAIDER. Maximal amplification occurs at an (emission) altitude where the two components have sufficiently separated in energy though not yet separated too strongly in space.     

One zone modeling of irregular variability of stellar convective envelope

One zone modeling of the irregular variability of red super-giants is intended with regard to the nonlinear coupling of finite amplitude pulsation with convection. The nonlocal mixing length is employed for the evaluation of the convective flux, the turbulent pressure and the turbulent power of temperature fluctuations. The radial pulsation and the Boussinesq convection are assumed for simplicity. The one zone is defined as the layer having the entropy maximum and the minimum at the bottom and at the top, respectively. The quasi-adiabatic approximation is consistent with this definition in fixing the zone to the same mass range. The spatial derivatives are evaluated under the assumption of homologous changes with the equilibrium homologous parameters. Then, a set of 6 simultaneous first order nonlinear ordinary differential equations are obtained as the one zone representation of the irregular variability of the convective envelope.     

An Emulation Research on the Radio Occultation Exploration of Martian Ionosphere

The technical system of the Sino-Russian joint satellite-to-satellite Mars ionosphere occultation is analyzed and introduced. The analogue computation of the observed values of the radio waves of the ionosphere occultation event is carried out by adopting the three-dimensional ray tracking method and the electron density profile inversion is conducted by means of the simulated occultation observational data, with the result showing that the emulation algorithm is reliable. By taking advantage of the emulation method the case computation and analysis of the inversion errors caused by the observational error of the occultation radio wave phase and the satellite orbital error are respectively carried out, and it is obtained from the result that the effect of the phase measuring error of the 5% circle on the result of the daytime ionosphere occultation exploration may be neglected, while the absolute error of the night electron density measurement is less than 4 × 108 m^?3, and the main effect of the satellite orbital error on the occultation leads to the lifting or falling of the ionospheric height. The result shows that the technical system of the Sino-Russian joint Mars ionosphere occultation exploration is advanced. It can be expected that the high accuracy electron density profile is obtained and the technical system can be applied to the exploration of the lunar ionospheric environment.     

青岛海陆风三维结构的数值模拟

本文采用 1个陡地形影响修正的三维中尺度流体静力的气象学模式 ,对青岛地区海陆风的日变化规律和三维结构进行了较细致的分析。结果显示 ,青岛有多支海陆风存在 ,且每支海陆风出现的时间、强度和向内陆伸展的距离有很大的不同。这其中沿岸山地的机械和热力作用扮演着重要的角色。在观测站 ,模拟结果和实测资料等方面有较好的一致性。     

A Statistical Study of Rapid Sunspot Structure Change Associated with Flares

We reported recently some rapid changes of sunspot structure in white-light(WL) associated with major flares.We extend the study to smaller events and present here results of a statistical study of this phenomenon.In total,we investigate 403 events from 1998 May 9 to 2004 July 17,including 40 X-class,174 M-class,and 189 C-class flares.By monitoring the structure of the flaring active regions using the WL observations from the Transition Region and Coronal Explorer(TRACE),we find that segments in the outer sunspot structure decayed rapidly right after many flares;and that,on the other hand,the central part of sunspots near the flare-associated magnetic neutral line became darkened.These rapid and permanent changes are evidenced in the time profiles of WL mean intensity and are not likely resulted from the flare emissions.Our study further shows that the outer sunspot structure decay as well as the central structure darkening are more likely to be detected in larger solar flares.For X-class flares,over 40% events show distinct sunspot structure change.For M-and C-class flares,this percentage drops to 17% and 10%,respectively.The results of this statistical study support our previously proposed reconnection picture,i.e.,the flare-related magnetic fields evolve from a highly inclined to a more vertical configuration.     

湘东锡田地区太和仙金多金属矿找矿潜力分析

文章通过对太和仙金多金属矿区地层、构造、岩浆岩、矿体特征等的综合研究与分析,认为该矿区矿源层分布广泛,成矿构造条件优越,成矿序列明显,矿床属岩浆热液成因的破碎带蚀变岩型金多金属矿床,并以此为基础,建立了太和仙矿区破碎带蚀变岩型金多金属矿的成矿模式;重力异常特征、水系沉积物异常特征显示矿区处于隆起的热液活动区,下伏可能存在一隐伏岩体。推测太和仙矿区找矿潜力大,可作为寻找中大型以上规模金多金属矿床的有利地段。     

中国城市群热岛效应时空演变及其影响因素分析

基于长期不透水面和MODIS地表温度数据,分析2000—2015年中国城市群扩张及热岛效应时空演变,进而综合采用冗余分析(RDA)、线性回归分析和变异分配分析(VPA)等方法,揭示城市群城市热岛效应的驱动机制。结果表明：城市群内建成区面积快速扩张,不透水面比例从2000年2.08%增长到2015年5.33%,且主要集中于珠江三角洲等沿海城市群;2000—2015年,夏季热岛分布较广,且白天强度高于夜晚。东部以及大部分北部城市群如哈长城市群等,降温强度较大,但其夜晚热岛效应在不同程度增强。冬季夜晚比白天热岛分布广、强度高,北方、西北、东部等地区夜晚热岛效应也在增强;自然环境因素显著影响城市群热岛强度,降水对夏季夜晚热岛强度起显著负贡献(22%),纬度越高,冬季夜晚热岛强度也越高。人为因素显著影响夜晚热岛分布和城市群内热岛强度的平衡,城市植被覆盖显著减少夜晚城市群内热岛分布,灯光强度对夏季夜晚热岛强度起显著负贡献(24%),对热岛比例起显著正贡献(27%),人口密度对夏季夜晚热岛强度起显著负贡献(31%);自然环境因素对热岛强度的贡献占主导,而人为干扰因素对热岛比例的贡献占主导。     

黄河兰州段2018年汛期沉积物的磁学特征研究: 对古洪水重建的启示

现代洪水沉积物的沉积学特征研究是开展古洪水重建的一项基础工作.2018年黄河汛期洪水沉积物在兰州体育公园形成了一道天然堤.对该天然堤剖面的岩石磁学研究显示：沉积物中的磁性矿物既有磁铁矿,又有赤铁矿/针铁矿.磁化率、饱和等温剩磁、非磁滞剩磁、S-ratio和L-ratio等参数在剖面上没有明显变化,指示2018年洪水沉积物源区、磁性矿物的种类和含量变化不显著.剖面下部（66~110 cm）沉积物的磁化率各向异性（AMS）椭球最大轴偏角集中分布（K₁-Dec=22.8°±10.3°）,上部（0~64 cm）沉积物的磁化率最大轴偏角在上半平面内随机分布;下部沉积物的磁性矿物粒度指标（χ_ARM/χ和χ_ARM/SIRM）和天然剩磁（NRM）强度低于上部;指示洪水沉积物的下部和上部分别形成于2018年黄河二号和三号洪水期间.由于二号洪水流量及水位陡升陡降、持续时间短,三号洪水水位升降相对缓慢、持续时间长;造成了两次洪水沉积物的AMS特征、χ_ARM/χ、χ_ARM/SIRM以及NRM强度差异.本研究揭示洪水沉积物的磁学参数能够灵敏地响应不同水动力条件和持续时间的洪水期次,从而具有高分辨率区分洪水事件的潜力.