The origin of our galactic magnetic field

A serious difficulty with the standard alpha‐omega theory of the origin of galactic magnetic fields involves the question of flux expulsion. This is intimately related to flux freezing. The alpha‐omega theory is shown in the context of the giant superbubble explosions that have a large impact on the physics of the interstellar medium. It is shown that superbubbles alone can duplicate the processes of the alpha‐omega dynamo and produce exponential growth of the galactic magnetic field. The possibility of the blow‐out of pieces of the magnetic field is discussed and it is shown that they have the potential to solve the flux‐expulsion problem. However, such an explanation must lead to apparent ‘gaps’ in the field in the galactic disc. These gaps are probably unavoidable in any dynamo theory and should have important observable consequences, one of which is an explanation for the escape of cosmic rays from the disc (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Large‐scale magnetic flux concentrations from turbulent stresses

In this study we provide the first numerical demonstration of the effects of turbulence on the mean Lorentz force and the resulting formation of large‐scale magnetic structures. Using three‐dimensional direct numerical simulations (DNS) of forced turbulence we show that an imposed mean magnetic field leads to a decrease of the turbulent hydromagnetic pressure and tension. This phenomenon is quantified by determining the relevant functions that relate the sum of the turbulent Reynolds and Maxwell stresses with the Maxwell stress of the mean magnetic field. Using such a parameterization, we show by means of two‐dimensional and three‐dimensional mean‐field numerical modelling that an isentropic density stratified layer becomes unstable in the presence of a uniform imposed magnetic field. This large‐scale instability results in the formation of loop‐like magnetic structures which are concentrated at the top of the stratified layer. In three dimensions these structures resemble the appearance of bipolar magnetic regions in the Sun. The results of DNS and mean‐field numerical modelling are in good agreement with theoretical predictions. We discuss our model in the context of a distributed solar dynamo where active regions and sunspots might be rather shallow phenomena (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Population study of Pectinaria australis (polychaeta) in Tasman Bay

Grab samples were taken from a population of Pectinaria australis Ehlers in Tasman Bay, New Zealand, at intervals over a 2‐year period, March 1971 to March 1973. Settlement occurred in summer with the new recruits showing rapid growth and heavy mortality, giving an apparent life cycle time of 1 y. The population density varied greatly over short distances at one time, presumably due to random settlement of aggregations of larvae from the plankton.     

Rainfall effect on wind waves and the turbulence beneath air-sea interface

Rainfall effects on wind waves and turbulence are investigated through the laboratory experiments in a large wind-wave tank. It is found that the wind waves are damped as a whole at low wind speeds, but are enhanced at high wind speeds. This dual effect of rain on the wind waves increases with the increase of rain rate, while the influence of rainfall-area length is not observable. At the low wind speed, the corresponding turbulence in terms of the turbulent kinetic energy （TKE） dissipation rate is significantly enhanced by rain- fall as the waves are damped severely. At the high wind speed, the augment of the TKE dissipation rate is suppressed while the wind waves are enhanced simultaneously. In the field, however, rainfall usually hin- ders the development of waves. In order to explain this contradiction of rainfall effect on waves, a possibility about energy transfer from turbulence to waves in case of the spectral peak of waves overlapping the inertial subrange of turbulence is assumed. It can be applied to interpret the damping phenomenon of gas trans- fer velocity in the laboratory experiments, and the variation of the TKE dissipation rates near sea surface compared with the law of wall.     

表面波浪对海洋上层混合的作用

A new three-dimensional numerical model is derived through a wave average on the primitive N-S equations, in which both the＂Coriolis-Stokes forcing＂ and the＂Stokes-Vortex force＂ are considered. Three ideal experiments are run using the new model applied to the Princeton ocean model （POM）. Numerical results show that surface waves play an important role on the mixing of the upper ocean. The mixed layer is enhanced when wave effect is considered in conjunction with small Langmuir numbers. Both surface wave breaking and Stokes production can strengthen the turbulent mixing near the surface. However, the influence of wave breaking is limited to a thin layer, but Stokes drift can affect the whole mixed layer. Furthermore, the vertical mixing coefficients clearly rise in the mixed layer, and the upper ocean mixed layer is deepened especially in the Antarctic Circumpolar Current when the model is applied to global simulations. It indicates that the surface gravity waves are indispensable in enhancing the mixing in the upper ocean, and should be accounted for in ocean general circulation models.     

Spectrum Analysis of Wind Profiling Radar Measurements

Unlike previous studies on wind turbulence spectrum in the planetary boundary layer, this investigation focuses on high-altitude （1-5 km） wind energy spectrum and turbulence spectrum under various weather conditions. A fast Fourier transform （FFT） is used to calculate the wind energy and turbulence spectrum density at high altitudes （1-5 km） based on wind profiling radar （WPR） measurements. The turbulence spectrum under stable weather conditions at high altitudes is expressed in powers within a frequency range of 2 × 10-5-10-3 s-1, and the slope b is between -0.82 and -1.04, indicating that the turbulence is in the transition from the energetic area to the inertial sub-range. The features of strong weather are reflected less obviously in the wind energy spectrum than in the turbulence spectrum, with peaks showing up at different heights in the latter spectrum. Cold windy weather appears over a period of 1.5 days in the turbulence spectrum. Wide-range rainstorms exhibit two or three peaks in the spectrum over a period of 15-20 h, while in severe convective weather conditions, there are two peaks at 13 and 9 h. The results indicate that spectrum analysis of wind profiling radar measurements can be used as a supplemental and helpful method for weather analysis.     

基于VOF方法的海底管道溢油扩散数值模拟研究

在海底输油管道运行过程中,管道渗漏、穿孔及破碎都会导致原油泄漏。对溢油运动的轨迹及其扩散范围作出预报可为溢油事故的处理提供及时、准确的信息,指导应急处理的正确实施。基于工程实际需求,采用有限体积法,结合k-ε紊流模型,建立了海流作用下海底输油管道溢油扩散数值模型。采用VOF方法(volume of fluid method)追踪多相流界面。首先,将数值模拟结果与Fan的实验值及Zheng和Yapa的数值结果进行了对比,验证数值模型的可靠性;其次,研究了不同原油溢出速度与环境水深对不同时刻溢油轨迹、到达海面时间、横向漂移距离与海面扩散范围的影响。研究表明:随原油溢出速度增大,溢油到达海面时间逐渐减小,溢油横向漂移距离与海面扩散范围则逐渐增大;随环境水深增大,溢油到达海面时间逐渐增大,且其变化接近线性分布。     

北京城郊近地层湍流实验观测

本文利用两台FA-11超声风速温度仪于1992年3月到４月间在北京325 m气象观测塔47 m和120 m两个高度观测到的风速三个正交分量以及声虚温的湍流脉动资料，计算和分析了北京城郊粗糙下垫面近地层湍流特征量及其日变化，无量纲垂直速度和声虚温的方差随稳定度的变化，风速分量和温度的归一化湍流能谱以及动量和热通量的互谱及其随稳定度的变化。并且与平坦均一下垫面近地层湍流观测的结果进行了对比。     

华南农田下垫面地气交换和能量收支的观测研究

利用2004年11月至12月在广东省惠州地区进行的湍流连续观测资料,分析非均匀农田近地面层的基本气象要素特征以及水汽和CO2的浓度与通量输送规律,作为今后深入探讨地表非均匀性效应的基础.通过各辐射分量和感热、潜热与土壤热通量的特征分析,研究能量收支的基本状况,并讨论了造成显著能量"不平衡"的原因.观测的基本结果是:(1)近地面1.8 m高度处以北风为主,风速大多低于2 m/s,正午入射太阳辐射约700 W/m2;CO2浓度的日变化范围为600～900 mg/m3,水汽为5～25 g/m3.(2)各气象要素呈现明显的日变化,当地温度日较差约10℃,相对湿度始终高于50%.CO2和水汽的浓度在夜间较白天高,二者的日平均值为713.7 mg/m3和15.9 g/m3;利用涡旋相关法,测得二者的通量在白天高于夜间,日平均值为25.3 mg·m-2·s-1和-4.7×10-2mg·m-2·s.当地的日平均波文(Bowen)比仅为0.04,这主要是由于当地的高湿度造成的.(3)当地存在显著的能量"不平衡"现象,正午时的差额热通量可高达150 W/m2,这可能与平均垂直运动输送的作用、观测误差以及通量和辐射观测的"源地"不匹配等原因有关.研究结果与荒漠、城市和稻田下垫面的观测事实进行了定量比较.     

Dimensionless measures of turbulent magnetohydrodynamic dissipation rates

The magnetic Reynolds number, R _M, is defined as the product of a characteristic scale and associated flow speed divided by the microphysical magnetic diffusivity. For laminar flows, R _M also approximates the ratio of advective to dissipative terms in the total magnetic energy equation, but for turbulent flows this latter ratio depends on the energy spectra and approaches unity in a steady state. To generalize for flows of arbitrary spectra we define an effective magnetic dissipation number,   R _M,e  , as the ratio of the advection to microphysical dissipation terms in the total magnetic energy equation, incorporating the full spectrum of scales, arbitrary magnetic Prandtl numbers, and distinct pairs of inner and outer scales for magnetic and kinetic spectra. As expected, for a substantial parameter range   R _M,e∼ O (1) ≪ R _M  . We also distinguish   R _M,e  from     where the latter is an effective magnetic Reynolds number for the mean magnetic field equation when a turbulent diffusivity is explicitly imposed as a closure. That   R _M,e  and     approach unity even if   R _M≫ 1  highlights that, just as in hydrodynamic turbulence, energy dissipation of large-scale structures in turbulent flows via a cascade can be much faster than the dissipation of large-scale structures in laminar flows. This illustrates that the rate of energy dissipation by magnetic reconnection is much faster in turbulent flows, and much less sensitive to microphysical reconnection rates compared to laminar flows.