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。     

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     

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。     

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.     

A possible explanation of photon emission from supernova remnants by jitter radiation

We investigate a possibility that non-thermal X-ray emission in a supernova remnant(SNR) is produced by jitter radiation, which is the analogue of synchrotron radiation in small-scale random magnetic fields. We can fit the multi-wavelength data of SNRs RX J1713.7-3946 (G347.3-0.5) and RX J0852.0-4622 (G266.6-1.2) by constructing pure jitter and inverse Compton (IC) emission models. We find that the physical fit parameters of random magnetic fields take values of several tens of μG strength and of the order of ∼10⁷ cm correlation length. These properties of random magnetic fields in collisionless shock of SNRs are discussed.      

阳江核电厂附近海域生物辐射影响评价研究

随着辐射防护理念的发展,环境中生物所受到的辐射影响日益引起人们的关注。本文使用ERICA项目中推荐的辐射影响评价方法,对阳江核电厂运行后对附近海域中海洋生物的辐射影响进行预测和评价。剂量率估算结果显示,阳江核电厂的液态放射性流出物对附近海域海洋生物造成的辐射剂量率不会超过7.47×10–3µGy.h–1,远低于国际上推荐的保护生物的辐射剂量率控制值,也低于本底辐射剂量率,因此,阳江核电厂正常运行后对附近海域中的海洋生物不会造成不利的辐射影响。