中国太阳总辐射的多元逐步回归模拟

研究采用年日照时数、年均总云量、年均水汽压、维度等常规气象要素及地理要素为解析变量,建立起估算全国范围内太阳年辐射总量的多元逐步回归模拟模型;利用全国730多个地面站1951—2002年间的常规气象观测资料,通过所构建的模型对中国太阳年辐射总量进行模拟分析,模型模拟分辨率为1km×1km,规模为4173×4847格网。模型数值计算结果显示:中国太阳辐射资源最丰富的地区为西藏自治区、青海东北部及甘肃西部边境等,高达6700MJ·m-2·a-1以上(一类地区),总面积约130万km2;最低的为四川盆地、青藏高原南部的雅鲁藏布峡谷地区,低于4200MJ·m-2·a-1(五类地区),总面积约75万km2;中国陆地表面每年接受的总太阳辐射能约为52.4×1018kJ;单位面积上太阳年辐射总量约介于2780—7560MJ·m-2·a-1;分布具有明显的地域性,呈现西北、北部高,东南、东部及东北的部分地区低的特点,模拟值较好拟合实际的太阳年辐射总量。研究所构建模型实现了太阳年辐射总量空间分布的连续模拟,模型在保证足够的模拟精度条件下,提高了运算效率,简化了模拟过程,适于全国尺度下太阳年辐射总量的数值模拟计算。     

煤体静载破坏微震、电磁辐射及裂纹扩展特征研究

为研究型煤在单轴压缩破裂过程中产生的微震、电磁辐射信号与裂纹演化特征的对应关系,利用自主设计的低噪声静态加载试验系统,对0～0.25、0.25～0.5、0.5～1.0、1～2 mm共4种不同粒度的型煤进行了单轴压缩破坏试验,同步采集了煤样破坏过程中的微震、电磁辐射信号及破坏视频图像,提出了一种煤体裂纹快速提取方法并计算了型煤裂纹面积的变化规律。研究结果表明:型煤在单轴压缩过程中产生的微震、电磁辐射信号及裂纹面积在时域上具有良好的同步性。型煤破坏过程中裂纹面积随时间变化曲线可分为4个阶段。第1阶段为压实阶段,煤样所受应力值较小,其表面的裂纹面积以极为缓慢的速率增加。第2阶段为初始破裂阶段,随着应力的增加和内部弹性势能的积聚,型煤表面裂纹面积的增加速率较压实阶段有明显提高,伴随产生许多细小裂纹。第3阶段为加速破裂阶段,随着应力继续增加以及材料内部积聚弹性能的释放,试样变形过程加速,导致裂纹面积增速进一步增大。第4阶段为卸压阶段,试样的裂纹面积达到最大值,承载能力急剧降低,发生失稳破坏。     

向下延拓航空重力数据的Tikhonov双参数正则化法

为了避免正则化参数对向下延拓过程可靠成分的修正影响,提出了Tikhonov双参数正则化法。引进截断参数,将法矩阵的奇异值分为相对较大的奇异值（可靠部分）和相对较小的奇异值（不可靠部分）;引进正则化参数,只对法矩阵的小奇异值进行修正,以抑制高频误差对向下延拓解的影响。采用改进的广义交互确认法（GCV）确定截断参数和正则化参数。基于EGM2008重力场模型仿真了一组航空重力数据,验证了该方法对航空重力数据向下延拓过程的有效性。     

地球内核快速旋转的发现与全球变化的轨道效应

科里奥利效应是产生内核快速旋转的主要原因。科氏力使上升物质向西漂移，下降物质向东漂移；造成地球外层自转减速，地球内层自转加速。所以，自旋体中的垂直运动可以产生大规模的水平运动——圈层差异旋转。地震波测量结果表明，内核旋转速度每年比地壳地幔快１°。对于一个内核差异旋转的地球，太阳辐射不仅形成地磁场的内外磁尾和地壳与内核的反向振动，而且影响核幔角动量交换和电磁耦合，从而控制了地球内能的释放，形成天文周期与地质旋回的一一对应关系。地球轨道和太阳轨道的全球变化响应，为太阳辐射量变化控制地球内能释放提供了证据     

数值模式中长波辐射参数化方案的对比试验

应用一个简化的长波辐射参数方案，与郭晓岚－钱永甫模式原有长波辐射参数化方案进行了对比，分析了它们对１００ｈＰａ，３００ｈＰａ，５００ｈＰａ，７００ｈＰａ及地面的高度场、温度场、流场及气压场模拟结果的影响，发现不仅两者结果相当一致，而且与实测结果也符合很好。     

塔克拉玛干沙漠腹地逐日太阳总辐射模拟计算 -以达理雅博依绿洲为例

基于塔克拉玛干沙漠腹地面积最大的天然孤立绿洲达理雅博依2015年1月—2016年2月太阳总辐射观测资料,运用H.L.Penman经验公式模拟计算了该地区2015年逐日总辐射累计量,模拟值与实测值的误差分析显示:本气候学方法成功模拟了沙漠腹地总辐射的年内变化趋势。使用模拟值估算得到达理雅博依绿洲2015年太阳总辐射累计量约为5 332.23 MJ·m-2。又以相同方法模拟了塔中气象站2015年3—5月总辐射变化,结果较达理雅博依的模拟更接近实测值,说明本模拟在塔克拉玛干沙漠腹地不同地点结果有效。     

Monte-Carlo Simulations of Cosmic-ray and Internal Radiation Effects on ISOCAM on Board ISO

One of the main limitations to the sensitivity of the infrared camera ISOCAM on-board the Infrared Space Observatory (ISO) comes from responsivity variations and glitches caused by the impacts of charged particles in photo-detectors. Glitch rate measurements, glitch properties and removal methods have already been addressed during the first ISO detector workshop(Madrid, 1998) and published in a special issue of Experimental Astronomy. It appeared that glitch rate and most of glitch properties could be reproduced by Monte-Carlo simulations. This is very interesting in order to predict before launch the effect of charged particles in photo-detectors operated in space. This paper presents results of Monte-Carlo simulations of radiation effects on ISOCAM detectors. Glitch rates, spatial and energetic properties of glitches have been computed and are compared with measured values. This revised version was published online in July 2006 with corrections to the Cover Date.     

Does the plasma composition affect the long-term evolution of relativistic jets?

We study the influence of the matter content of extragalactic jets on their morphology, dynamics and emission properties. For this purpose we consider jets of extremely different compositions, including pure leptonic and baryonic plasmas. Our work is based on two-dimensional relativistic hydrodynamic simulations of the long-term evolution of powerful extragalactic jets propagating into a homogeneous environment. The equation of state used in the simulations accounts for an arbitrary mixture of electrons, protons and electron–positron pairs. Using the hydrodynamic models, we have also computed synthetic radio maps and the thermal bremsstrahlung X-ray emission from their cavities.
Although there is a difference of about three orders of magnitude in the temperatures of the cavities inflated by the simulated jets, we find that both the morphology and the dynamic behaviour are almost independent of the assumed composition of the jets. Their evolution proceeds in two distinct epochs. During the first one, multidimensional effects are unimportant and the jets propagate ballistically. The second epoch starts when the first larger vortices are produced near the jet head, causing the beam cross-section to increase and the jet to decelerate. The evolution of the cocoon and cavity is in agreement with a simple theoretical model. The beam velocities are relativistic  ( Γ ≃4)  at kiloparsec scales, supporting the idea that the X-ray emission of several extragalactic jets may be due to relativistically boosted CMB photons. The radio emission of all models is dominated by the contribution of the hotspots. All models exhibit a depression in the X-rays surface brightness of the cavity interior, in agreement with recent observations.     

吸积盘谱讨论

本文用数值方法讨论了吸积盘谱与黑体谱的形状和谱指数。结果表明:对于吸积盘用F_v∝v~(1/3)作为其特征谱是不合适的;同时Frank等(1985)所得到的解析式F_v∝v~2也是不正确的。