超长La Ni?a事件背景下东亚夏季风的季节内变化:1999～2000年和1984～1985年的对比分析

基于多种再分析资料和观测资料,对比分析了两次超长La Ni?a事件中东亚夏季风的季节内变化。选取的两次事件分别发生在1984～1985年和1999～2000年,但强度有明显差异,其中前者为中等强度事件,而后者则为强事件。在两次事件过程中,暖池对流偏强,西太平洋副热带高压（副高）偏东偏弱,但季节内变化有很大差异。对强事件而言,6月对流开始发展,异常值在7月达到最大,8月稍弱,这与La Ni?a年合成结果一致,表明La Ni?a信号主导了东亚夏季风的季节内变化。与此不同的是,在1984～1985年事件中,6月和8月对流偏强,7月偏弱,呈双峰型异常变化。分析表明,当前一个月海温偏高时,后一个月对流偏强,减弱了太阳辐射,造成局地海温降低,偏低的海温又反过来抑制了后一个月的对流发展,暖池地区局地海气相互作用在中等强度La Ni?a事件中起到关键作用。因此,在两次超长La Ni?a事件中,东亚夏季风的季节内变化过程和影响因子有很大差异。此外,由于副高偏东,中国东部夏季降水总体上偏少。     

基于脉冲星计时的航天器自主定位误差估计方法

目前很多学者希望从"X射线脉冲星自主导航"的导航算法研究入手,利用数据分析或仿真进行验证.其中关于航天器自主定位的误差估计方法、误差量级和各种影响因素的讨论,并没有在给定详细初始条件的基础上系统性地说明问题.为了分析上述问题,需从天体测量学的角度出发,对自主定位的各种误差源及其影响因素进行探讨和误差量级的估计.首先,由...     

分块DPCM与5/3整数小波变换结合的天文图像无损压缩

针对海量的天文图像数据与有限的存储空间和带宽资源之间矛盾日益突出这一问题,提出一种无损压缩方法,首先将超大天文图像分块,再使用差分脉冲编码调制和5/3整数小波变换,最后使用霍夫曼算法编码。对该方法的原理和具体实现做了详细的分析与介绍,通过实验验证该方法比天文中常用的tar、PKZip、WinZip、WinRar软件在压缩比上分别提高了30%、29%、26%、2%,压缩速度远大于WinZip和WinRar;且该算法实现简单,适合硬件实现和利于并行处理。     

Stable Isotopes and Halogen Geochemistry of the Huayuan Carbonate-hosted Pb-Zn Ore District, South China: Implications for the Salt Source of Ore-forming Fluids

The Huayuan Pb-Zn ore district in China, located in western Hunan Province, is a giant carbonate-hosted Pb-Zn ore district. The source of ore-forming brines in this ore district remains poorly constrained. Whether the highly saline brines are derived from evaporated seawater or dissolved evaporates continues to be intensely debated. Carbonate minerals associated with Pb-Zn mineralization have δ13CV-PDB and δ18OV-SMOW values ranging from ?5.55‰ to +1.35‰ (mean value of ?0.69‰; n = 14) and +16.28‰ to +25.05‰ (mean value of +20.22‰; n = 14), respectively. This indicates that carbonate minerals are dominantly formed from dissolved ore-hosted carbonate rocks. The δ34S values of sulfides range from +20.2‰ to +36.8‰, with an average value of +30.0‰ (n = 27). These results suggest that sulfur is predominantly derived from the thermochemical sulfate reduction of marine sulfate. The crush-leach analyzed solute data of fluid inclusions in sphalerite show the ore-forming fluids have Cl/Br molar ratios range from 118 to 384, and Na/Br molar ratios from 39 to 160 (n = 8). These Cl/Br ratios of hydrothermal fluid are much lower than those of seawater (657 to 564), but are consistent with bittern brines through early halite precipitation. We propose that ore-forming fluids are mainly derived from evaporitic basin brines, which leached base metals from the basement and/or country rocks. The brine then migrated to the basin margins through clastic rocks of basement and then precipitated sul?des by thermochemical sulfate reduction.     

基于飞机观测资料的石家庄秋季对流层CH4垂直分布特征

为研究石家庄秋季对流层内CH₄垂直分布特征,2018年9月使用“空中国王350”飞机搭载Picarro温室气体在线观测仪和气象要素观测设备,对石家庄上空（600—5500 m）CH₄浓度进行探测。探测期间共飞行7架次,取得7条CH₄浓度廓线数据。结果表明: 石家庄上空近地面层（1000 m以下）CH₄平均浓度与同时间段区域背景站上甸子站CH₄浓度呈显著正相关（r=0.81,P < 0.03）。探测到的CH₄浓度最小值为1898×10^-9摩尔分数,最大值为2219×10^-9摩尔分数,平均浓度为1981×10^-9摩尔分数。观测得到的7条廓线均有较好的一致性,2000 m以上,浓度均随高度呈先增大后减小的趋势。利用后向轨迹模式（HYSPLIT）对探测时段内石家庄上空不同高度层主要气流传输路径进行统计分析表明,600 m高度输送路径较短,CH₄浓度受本地排放影响较大; 3000 m受输送作用影响较大,偏西和西南路径可能将较高CH₄浓度气团输送至石家庄上空; 5000 m气团传输对CH₄浓度影响较小,浓度相对较稳定,对传输路径的变化不敏感。     

The heating of the solar transition region

The temperature curve in the solar chromosphere has puzzled astronomers for a long time.Referring to the structure of supergranular cells,we propose an in ductive heating model.It mainly includes the following three steps.(1) A small-scale dynamo exists in the supergranulation and produces alternating small-scale magnetic fluxes;(2) The supergranular flow distributes these small-scale fluxes according to a regular pattern;(3) A skin effect occurs in the alternating and regularly-distributed magnetic fields.The induced current is concentrated near the transition region and heats it by resistive dissipation.     

Multi-band optical variability of BL Lac object OQ 530

Historical optical data are combined on the BL Lac object OQ 530.Verifying the existence of correlations among the flux variations in different bands serves as an important tool to investigate emission processes.To examine the possible existence of a lag between variations in different optical bands from this source,a statistical analysis is performed through the discrete correlation function(DCF)method and the z-transformed discrete correlation function(ZDCF)method.Monte Carlo simulations called"flux redistribution/random subset selection"(FR/RSS)are performed to obtain statistically meaningful values for the cross-correlation time lags and their related uncertainties.The analysis confirms that the variations in different optical light curves are strongly correlated,with zero-lag within the errors.Long term variability of color indexes is also analyzed.The result suggests a strong correlation between color index and brightness.A clear bluer-when-brighter chromatism is found,in the sense that the spectrum steepens as the brightness decreases.     

The “Same Side – Opposite Side Effect” of the Heliospheric Current Sheet in Ionospheric Negative Storms

Using 141 CME-interplanetary shock (CME-IPS) events and foF2 from eight ionosonde stations from January 2000 to September 2005, from the statistical results we find that there is a “same side?–?opposite side effect” in ionospheric negative storms, i.e., a large portion of ionospheric negative disturbances are induced by the same-side events (referring to the CMEs whose source located on the same side of the heliospheric current sheet (HCS) as the Earth), while only a small portion is associated with the opposite-side events (the CMEs source located on the opposite side of the HCS as the Earth); the ratio is 128 vs. 46, and it reaches 41 vs. 14 for the intense ionospheric negative storms. In addition, the ionospheric negative storms associated with the same-side events are often more intense. A comparison of the same-side event (4 April 2000) and the opposite-side event (2 April 2001) shows that the intensity of the ionospheric negative storm caused by the same-side event is higher than that by the opposite-side event, although their initial conditions are quite similar. Our preliminary results show that the HCS has an “impeding” effect to CME-IPS, which results in a shortage of energy injection in the auroral zone and restraining the development of ionospheric negative perturbations.     

AMR Simulations of Magnetohydrodynamic Problems by the CESE Method in Curvilinear Coordinates

The objective of this paper is to present new extensions of the space – time conservation element and solution element (CESE) method for simulations of magnetohydrodynamic (MHD) problems in general curvilinear coordinates by using an adaptive mesh refinement (AMR) grid system. By transforming the governing MHD equations from the physical space (x,y,z) to the computational space (ξ,η,ζ) while retaining the form of conservation, the CESE method is established for MHD in the curvilinear coordinates. Utilizing the parallel AMR package PARAMESH, we present the first implementation of applying the AMR CESE method for MHD (AMR-CESE-MHD) in both Cartesian and curvilinear coordinates. To show the validity and capabilities of the AMR-CESE-MHD code, a suite of numerical tests in two and three dimensions including ideal MHD and resistive MHD are carried out, with two of them in both Cartesian and curvilinear coordinates. Numerical tests show that our results are highly consistent with those obtained previously by other authors, and the results under both coordinate systems confirm each other very well.     

The Contribution from Radio Quiet Quasars to γ-ray Background

The EGRET observations have confirmed and proposed the new isotropically distributed γ-ray background, but the known objects radiating γ-rays can not supply so much radiation. Meanwhile, EGRET also reveals a population of γ-ray sources with no radio counterparts which are isotropically distributed in the sky, indicating their possible cosmological origins. Wang et al.^[13] proposed a new γ-ray radiation process driven by the radiation feedback of AGNs. The energy of the radiation peaks around 1 GeV—0.1 TeV with the typical luminosity of 10⁴²—10⁴³ ergs · s^?1. This kind of radiation process in the radio quiet quasars make them the potential γ-ray radiation sources as well as the contributors to the γ-ray background. We consider two cases in which the seed photons in the inverse-Compton processes are from the accretion disks of quasars and cosmic microwave background (CMB), respectively. We find that the former contributes 78%—92% of the background radiation around 1 GeV, while the contribution from the latter is negligible. The radio quiet quasars are highly likely to become the objects which contribute the most energy to the γ-ray background around 1 GeV.