河北春季一次飞机人工增雪的综合分析   总被引：1，自引：0，他引：1  

李宝东  孙玉稳  孙霞  刘伟  韩洋  蒋元华 《干旱气象》2014,(5):819-829

2013年4月19日,河北省人工影响天气办公室在河北中南部地区根据云系特点首次采用多层次水平催化和垂直验证的方式对层状云进行人工催化和探测。本文利用机载仪器所取得的飞机探测资料,结合实时天气、卫星、雷达、探空和雨量观测资料,分析了河北春季层状云增雪作业的技术指标,探讨了航测微物理参量和卫星、雷达、探空等资料在作业中的应用。结果表明：云在发展期雷达回波由15 dBZ逐步上升到25-35 dBZ,卫星反演的云顶高度、云顶温度、有效粒子半径、光学厚度等都有增加;云在中后期有效粒子半径、光学厚度、液水路径迅速下降,雷达回波同时减弱。在高度3 177-5 723 m之间过冷云滴达100-700个/cm^3,含水量在0.01 g·m^-3左右,最大0.081 g·m^-3,云粒子主要在此增长,形成降水粒子,该区间适宜催化。作业后,影响区内云体发展,雷达回波增强,出现35 dBZ强回波,且强回波中心扩大;卫星反演的云顶高度、光学厚度等比对比区有明显增加。  相似文献   

光衰减系数与悬浮颗粒物浓度的关系     

王鲁宁  魏皓  赵亮 《中国海洋大学学报(自然科学版)》2014,44(4):8-14

海水中光合作用有效光强(PAR)的变化受多种因素影响,其中分布在海水中的悬浮颗粒物是造成PAR在水中衰减的重要因素之一,尤其是在风与潮混合作用较强的近海。已有的研究表明:PAR在水中是呈指数衰减的,并且在悬浮物颗粒物分布比较稳定时,光衰减系数k与悬浮物体积浓度线性相关。在生态模型中,往往需要利用k获得水下光强,而衰减系数k很难直接通过观测得到,因此本文目的就是建立衰减系数与悬浮颗粒物体积浓度的关系,后者可通过观测得到。经过对2个航次与2个定点观测数据的处理,得到了PAR衰减系数分别与所有粒径悬浮物颗粒物总体积浓度以及3种粒级(黏土、粉砂、细砂)悬浮物体积浓度之间的线性关系式,并且发现相对于细砂,较小粒径的黏土、粉砂的浓度能更好的表征PAR的衰减特性。  相似文献   

Regular and chaotic dynamics in 3D reconnecting current sheets     

C. Gontikakis  C. Efthymiopoulos  A. Anastasiadis 《Monthly notices of the Royal Astronomical Society》2006,368(1):293-304

We consider the possibility of particles being injected at the interior of a reconnecting current sheet (RCS), and study their orbits by dynamical systems methods. As an example we consider orbits in a 3D Harris type RCS. We find that, despite the presence of a strong electric field, a 'mirror' trapping effect persists, to a certain extent, for orbits with appropriate initial conditions within the sheet. The mirror effect is stronger for electrons than for protons. In summary, three types of orbits are distinguished: (i) chaotic orbits leading to escape by stochastic acceleration, (ii) regular orbits leading to escape along the field lines of the reconnecting magnetic component, and (iii) mirror-type regular orbits that are trapped in the sheet, making mirror oscillations. Dynamically, the latter orbits lie on a set of invariant KAM tori that occupy a considerable amount of the phase space of the motion of the particles. We also observe the phenomenon of 'stickiness', namely chaotic orbits that remain trapped in the sheet for a considerable time. A trapping domain, related to the boundary of mirror motions in velocity space, is calculated analytically. Analytical formulae are derived for the kinetic energy gain in regular or chaotic escaping orbits. The analytical results are compared with numerical simulations.  相似文献   

11颗行星际尘粒中的锂,硼同位素丰度分析     

谢萍 《紫金山天文台台刊》1997,16(2):77-81

我们首次测量了4颗行星际尘粒(IDPs)中的~6Li/~7Li,~(10)B/~(11)B。它们的平均值分别是(8.40±0.37)×10~(-2)和(2.40±0.18)×10~(-2),随后又精确测量了7颗IDPs~6Li/Li的同位素丰度。  相似文献   

The Photon Mean Free Path Sphere, The Minimum Energy, and the Masses of the Main Elementary Particles     

A. Dinculescu 《Astrophysics and Space Science》2006,301(1-4):153-155

The photon mean free path sphere has several properties that strongly correlate with characteristics of the observable universe. This apparent connection led to a set of equations that were recently used to derive the values of the main cosmological parameters. It also leads, via an expression for the minimum energy, to an equation relating the mass of the proton to the mass of the electron.  相似文献   

Pair emission from bare magnetized strange stars     

D. B. Melrose  R. Fok †  D. P. Menezes ‡ 《Monthly notices of the Royal Astronomical Society》2006,371(1):204-210

The dominant emission from bare strange stars is thought to be electron–positron pairs, produced through spontaneous pair creation (SPC) in a surface layer of electrons tied to the star by a superstrong electric field. The positrons escape freely, but the electrons are directed towards the star and quickly fill all available states, such that their degeneracy suppresses further SPC. An electron must be reflected and gain energy in order to escape, along with the positron. Each escaping electron leaves a hole that is immediately filled by another electron through SPC. We discuss the collisional processes that produce escaping electrons. When the Landau quantization of the motion perpendicular to the magnetic field is taken into account, electron–electron collisions can lead to an escaping electron only through a multistage process involving higher Landau levels. Although the available estimates of the collision rate are deficient in several ways, it appears that the rate is too low for electron–electron collisions to be effective. A simple kinetic model for electron–quark collisions leads to an estimate of the rate of pair production that is analogous to thermionic emission, but the work function is poorly determined.  相似文献   

The Influence of Ion-Acoustic Turbulence on the Electron Acceleration in the Reconnecting Current Sheet     

Gui-Ping Wu  Guang-Li Huang  Yu-Hua TangDepartment of Physics  Southeast University  Nanjing  Purple Mountain Observatory  Chinese Academy of Sciences  Nanjing Department of Astronomy  Nanjing University  Nanjing 《中国天文和天体物理学报》2005,5(1):99-109

Through solving the single electron equation of motion and the Fokker-Planck equation including the terms of electric field strength and ion-acoustic turbulence, we study the influence of the ion-acoustic wave on the electron acceleration in turbulent reconnecting current sheets. It is shown that the ion-acoustic turbulence which causes plasma heating rather than particle acceleration should be considered. With typical parameter values, the acceleration time scale is around the order of 10^-6 s, the accelerated electrons may have approximately a power-law distribution in the energy range 20 ～100 keV and the spectral index is about 3～10, which is basically consistent with the observed hard X-ray spectra in solar flares.  相似文献   

Magnetic jets from swirling discs     

D. Lynden-Bell 《Monthly notices of the Royal Astronomical Society》2006,369(3):1167-1188

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Relativistic Fermi acceleration with shock compressed turbulence     

Martin Lemoine  Benoît Revenu 《Monthly notices of the Royal Astronomical Society》2006,366(2):635-644

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Shock surfing acceleration   总被引：1，自引：0，他引：1  

Vitali D Shapiro  Defne Üçer 《Planetary and Space Science》2003,51(11):665-680

Analytical and numerical analysis identify shock surfing acceleration as an ideal pre-energization mechanism for the slow pick-up ions at quasiperpendicular shocks. After gaining sufficient energy by shock surfing, pick-up ions undergo diffusive acceleration to reach their observed energies. Energetic ions upstream of the cometary bow shock, acceleration of solar energetic particles by magnetosonic waves in corona, ion enhancement in interplanetary shocks, generation of anomalous cosmic rays from interstellar pick-up ions at the termination shock are some of the cases where shock surfing acceleration apply. Inclusion of the lower-hybrid wave turbulence into the laminar model of shock surfing can explain the preferential acceleration of heavier particles as observed by Voyager at the termination shock. At relativistic energies, unlimited acceleration of ions is theoretically possible; because for sufficiently strong shocks main limitation of the mechanism, caused by the escape of accelerated particles downstream of the shock during acceleration no longer exists.  相似文献