日食一厄尔尼诺系数及其应用

通过比较本世纪以来的厄尔尼诺年和日食资料,发现了高纬（包括极区）日食与厄尔尼诺年之间存在着一定的因果关系。通过定义年日食一厄尔厄诺系数Ｒ１和累积日食一厄尔尼诺系数Ｒ２后,可以发现当某年的Ｒ１≥９或Ｒ２≥１０．５级时,则当年必为厄尔尼诺年,反之亦然．本文还提出了日食诱发厄尔尼诺现象的热一动力机制,并预测２０００年将是一个强厄尔尼诺年．     

利用卫星遥感资料估算海面太阳辐照度的初步结果

本文在分析了若干由卫星信息提取地表的太阳辐照度物理模式的基础上,将１９９５年５月２６日的ＮＯＡＡ卫星ＡＶＨＲＲ资料经适当变换后,选用Ｈａｙ和Ｈａｎｓｏｎ模式估算并分析了黄渤海３５°～４０°Ｎ、１２０°～１２５°Ｅ海区的海面太阳辐照度值。文中指出,卫星测量可成为海面太阳辐照度观测的有效手段。建议：１）尽快在国内开展这方面的研究;２）应进行海洋实况测量（最好是卫星过境时同步进行）;３）建立从卫星资料提取我国海区海面辐照度的适用算法。     

鲁西北地区鱼塘水体反射率

太阳短波辐射反射率与水体理化特性关系密切,鱼塘水体除具有一般水体反射率特性外,还与鱼塘澡浮游植物一道量存在的良好的负相关。在一定温度条件下,浮游植物的生长速度与光合有效辐射呈正相关,而随着浮游植物的增加,又降低了太阳辐射的反射效应,从而水体对光合有效辐射的吸收,随着浮游植物的增加而增加。     

地磁活动对气候要素影响的研究进展

地磁活动是太阳爆发现象引起地球近地空间磁场扰动的重要空间天气过程之一.地球磁场的变化具有多种时间尺度,其中从数十年到数世纪的长时间地磁场变化主要是由地核磁场引起的,而从数秒到数年的短时间地磁变化与太阳活动有关.近年来,越来越多的统计研究表明,地磁活动与太阳活动和地球气候变化之间存在着显著的相关性.地球磁场和地球大气系统的耦合现象驱动着人们探索地磁活动对地球天气和气候系统影响的研究.本文的目的就是综述国内外地磁变化对气候影响的研究进展,介绍我们最新的研究成果,探索地磁活动对气候要素的影响特征和可能机理过程,为深入研究地磁活动对地球天气和气候的影响提供基础和依据,以期对地磁活动和气候要素关系有进一步的认识.     

Numerical simulations of the magnetic field distribution in a solar complex of activity

Powerful solar complexes of activity are supposed to result from the excitation of Rossby vortices within a thin layer beneath the convection zone. Numerical simulations demonstrate that Rossby vortices generate large-scale arc-like magnetic structures. It is shown that the most powerful complex of activity observed in June-July 1982 was likely to be a result of the excitation of a Rossby anticyclone rather than a cyclone.     

Meridional circulation from differential rotation in an adiabatically stratified solar/stellar convection zone

Meridional circulation in stellar convection zones is not generally well observed, but may be critical for the workings of MHD dynamos operating in these domains. Coriolis forces from differential rotation play a large role in determining what the meridional circulation is. Here, we consider the question of whether a stellar differential rotation that is constant on cylinders concentric with the rotation axis can drive a meridional circulation. Conventional wisdom says that it can not. Using two related forms of the governing equations that respectively estimate the longitudinal components of the curl of the meridional mass flux and the vorticity, we show that such differential rotation will drive a meridional flow. This is because to satisfy anelastic mass conservation, non-spherically symmetric pressure contours must be present for all differential rotations, not just ones that depart from constancy on cylinders concentric with the rotation axis. Therefore, the fluid is always baroclinic if differential rotation is present. This is because, in anelastic systems, the perturbation pressure must satisfy a Poisson type equation, as well as an equation of state and a thermodynamic equation. We support our qualitative reasoning with numerical examples, and show that meridional circulation is sensitive to the magnitude and form of departures from rotation constant on cylinders. The effect should be present in 3D global anelastic convection simulations, particularly those for which the differential rotation driven by global convection is nearly cylindrical in profile. For solar-like differential rotation, Coriolis forces generally drive a two-celled circulation in each hemisphere, with a second, reversed flow at high latitudes. For solar like turbulent viscosities, the meridional circulation produced by Coriolis forces is much larger than observed on the Sun. Therefore, there must be at least one additional force, probably a buoyancy force, which opposes the meridional flow to bring its amplitude down to observed values.     

Incorporating velocity shear into the magneto-Boussinesq approximation

Motivated by consideration of the solar tachocline, we derive, via an asymptotic procedure, a new set of equations incorporating velocity shear and magnetic buoyancy into the Boussinesq approximation. We demonstrate, by increasing the magnetic field scale height, how these equations are linked to the magneto-Boussinesq equations of Spiegel and Weiss (Magnetic buoyancy and the Boussinesq approximation. Geophys. Astrophys. Fluid Dyn. 1982, 22, 219–234).     

地震台站新型太阳能供电系统设计

在虎门地震综合观测站的建设中,设计了一套以太阳能为主、发电机为辅的新型供电系统,解决了工作人员日常照明及地震仪器设备的交、直流用电问题。本文主要介绍该太阳能供电系统的设计过程。     

小行星深空探测的科学意义和展望

太阳系深空探测活动方兴未艾,小行星探测已成为主要发展方向。通过回顾近年来几个主要的国际小行星空间探测计划以及取得的研究成果,总结了小行星深空探测从早期的近距离飞越到小行星低空绕轨勘探,到目前的表面软着陆和采集样品返回的发展进程。同时深空探测也给行星科学研究者提出了新的挑战,鉴于目前行星科学的研究热点,详细叙述了小行星深空探测急需解决的重大科学问题及其科学意义,随后简单介绍了未来小行星深空探测计划的科学目标,为小行星深空探测的具体任务提供了科学目标选择方向。最后呼吁我国及时介入小行星深空探测,提升航天能力,开拓深空领域。     

太阳X-EUV成像望远镜

太阳X_EUV成像望远镜用来监测和预报影响空间天气变化的太阳活动,专门服务于空间天气预报研究. 望远镜工作在4～100?的X射线波段和195?极紫外谱段,视场角45′,角度分辨5″,提供全日面、高分辨的成像观测. 文中分析了太阳X、EUV波段的成像观测应用,介绍了X_EUV望远镜的基本设计,分析了望远镜对不同温度日冕等离子体的敏感性、对不同太阳活动现象的响应及反演日冕等离子体参数过滤片的组合利用. 太阳X_EUV成像望远镜集成了掠入射望远镜和正入射望远镜两套系统,扩展了单一X射线望远镜的成像功能,能够观测更多的太阳爆发先兆现象或者伴生现象,是目前国际上同类仪器中最新的太阳成像监测仪器.