海雾过程中大气气溶胶谱变化及消光作用

海雾是沿海地区的常见天气,大雾致灾的现象时有发生,然而对海雾微物理过程的研究相对匮乏。本文以北方的1次海雾过程为例,分析在雾的生成、维持和加强阶段气溶胶谱的变化、消光作用和对能见度的影响。发现暖湿气流影响下,空气比湿持续增加是1μm以上粗粒子数浓度增加的主要原因,比湿持续增加的速度越快,粒子数浓增长的幅度也越大,对能见度的影响也越大。反之,如果比湿持续下降,1~2.5μm粒子数浓度就会减小,能见度增加。粒子直径的增长速率在10-5(μm/s)量级以内。低能见度出现的时间与1~5μm粒子浓度相关性最好,低能见度发生的时间基本上与1~5μm粒子浓度开始增加的时间相一致。在雾的维持阶段小粒子通过增长被消耗,而较大粒子被雾滴清除。在雾的加强阶段,大粒子的增长速度超过了雾滴的清除。雾过程中以大于0.5μm粒子的消光作用为主,消光系数变化与能见度变化有很好的反相关关系,并且粒径越大,反相关关系越好。     

海雾生成过程中平流、湍流和辐射效应的数值试验

利用相对湿度方程,结合数值模式研究了在海雾生成过程中平流、湍流和辐射的效应。结果表明,海雾生成的主要“推动力”是长波辐射冷却,湍流冷却在低层主要发生在平流的初始阶段。随着时间的推移,湍流对低层大气很快变为起加热作用,不利于海雾的生成。湍流和辐射效应在低层大气中符号相反(仅在海雾生成的初始阶段符号相同),量级相同,在高层大气中湍流和辐射效应符号相同,但辐射效应占优势。湍流效应和辐射效应是影响海雾生成的主要因素,平流直接作用似乎不大。平流、湍流和辐射效应及其总效应均随时间推移而减小。另外,还初步研究了风速大小和海温高低对平流、湍流和辐射效应及海雾生成的影响。     

利用地物光谱仪数据研究水汽对太阳辐射的吸收

论文将在介绍太阳辐射衰减理论的基础上,利用地物光谱仪、太阳辐射计和臭氧监测仪测量所得到的海面入射的太阳直射辐射光谱数据及大气衰减数据,提出了一种研究水汽在近红外波段对太阳辐射吸收作用的新方法,利用该方法得到的水汽吸收系数与前人研究结果非常一致。在可见光波段,大气对太阳辐射的吸收主要体现为臭氧的吸收。在近红外波段,臭氧的吸收非常小,对大气起吸收作用的主要为水汽。     

紫外光对有毒甲藻塔玛亚历山大藻的生态学效应

对1991年分离自南海大鹏湾海域的塔玛亚历山大藻单克隆培养林在不同光照条件、辐射强度（9.5，5．9W／m2）（辐射剂量为：95，190，380,760,1520J/m2）和营养盐（N，P）浓度下，进行紫外辐射敏感性的研究。结果表明，紫外辐射可以导致细胞变形、增大和死亡。不论在什么条件下，低剂量的紫外辐射（95J／m2）就能使该藻的存活率和生长率大幅下降。此后，随着辐射剂量的增加，虽然存活率和生长率继续下降，但下降幅度渐缓。充足的营养盐和辐射处理后的连续光照对藻群的恢复有益，但在缺氮和缺磷条件下培养的藻群，可能由于生理活性减弱而导致对紫外辐射敏感性的迟钝。辐射强度对该藻的紫外辐射敏感性的影响十分显著，而且与辐射剂量具有明显的双重效应。     

Possible origin of clusters in ultra-high-energy cosmic rays

We estimate the detection rate of ultra-high-energy cosmic rays on ground-based arrays by assuming that the cosmic-ray sources are active galactic nuclei. We analyze the cases of detection of clusters, several particles that arrived, within the error limits, from the same area of the sky. The adopted model is shown to explain the detection rate of clusters on the AGASA array.     

变化磁场中相对论电子系集体的共振逆康普顿散射谱

强磁场中的共振逆康普顿散射(RICS)是产生伽玛射线的有效机制．在前文工作的基础上，导出强磁场中子星中具有幂律能谱的大量相对论电子沿中子星磁轴向外运动时在变化磁场中产生的集体RICS辐射谱(RICS谱光度)的基本公式．由此得到在中子星周边几种典型的低频辐射场中集体RICS辐射谱形的简单解析表示(如热轫致辐射场、黑体辐射场，以及非热低频幂律谱辐射场)，以便与实际观测谱形比较．计算表明：在满足匹配条件(即近似共振条件)下，RICS辐射效率很高，其谱形都是两段式(折断的)的幂律谱形式，与周边低频场性质无关．通过计算，再一次论证RICS机制是伽玛射线脉冲星和伽玛暴(GRBs)在高能射线段(硬X-射线和伽玛射线)辐射的一个理想的高效辐射机制。     

Photon scattering in the solar ultraviolet lines of He i and He ii

Observations made with the Coronal Diagnostic Spectrometer (CDS) onboard the Solar and Heliospheric Observatory ( SOHO ) are used to investigate the behaviour of the intensities of the emission lines of He  i , He  ii and O  iii at the quiet Sun-centre and at  θ= 60°  towards the equatorial limb. The aim is to examine the possible effects of photon scattering on the spatial variation of the optically thick helium lines. At the quiet Sun-centre, we find that, in agreement with previous work, the ratios of the intensities of the He  i 584-Å and He  ii 304-Å lines to those of the O  iii 600-Å line decrease systematically as the intensity of the O  iii line increases. However, we find that the dependence of these ratios on the O  iii intensity is not unique, but differs between the individual regions studied. Similar results are found at  θ= 60°  . We have also used line intensities and intensity ratios to investigate limb-to-disc effects and variations across a sample of supergranulation cell boundaries and adjacent cell interiors at both locations. The results do not exclude photon scattering as the cause of the larger observed ratios in cell interiors. The differences between the apparent widths of boundaries in O  iii at Sun-centre and 60° show that the emitting material is extended in height, which will aid the process of scattering into cell interiors. Photon scattering could also account for the lack of oscillations in the He  i intensities in a cell interior studied by Pietarila & Judge. Three-dimensional radiative transfer calculations in chosen geometries are now needed to account for the observations in detail.     

Radio signature of cosmological structure formation shocks

In the course of the formation of cosmological structures, large shock waves are generated in the intracluster medium (ICM). In analogy to processes in supernova remnants, these shock waves may generate a significant population of relativistic electrons which, in turn, produce observable synchrotron emission. The extended radio relics found at the periphery of several clusters and possibly also a fraction of radio halo emission may have this origin. Here, we derive an analytic expression for (i) the total radio power in the downstream region of a cosmological shock wave, and (ii) the width of the radio-emitting region. These expressions predict a spectral slope close to −1 for strong shocks. Moderate shocks, such as those produced in mergers between clusters of galaxies, lead to a somewhat steeper spectrum. Moreover, we predict an upper limit for the radio power of cosmological shocks. Comparing our results to the radio relics in Abell 115, 2256 and 3667, we conclude that the magnetic field in these relics is typically at a level of 0.1 μG. Magnetic fields in the ICM are presumably generated by the shocks themselves; this allows us to calculate the radio emission as a function of the cluster temperature. The resulting emissions agree very well with the radio power–temperature relation found for cluster haloes. Finally, we show that cosmic accretion shocks generate less radio emission than merger shock waves. The latter may, however, be detected with upcoming radio telescopes.