上海二次温室大棚区强尘卷风的成因分析     

戴蔚明  胡平  荣裕良  马忠芬  顾忠良 《气象科学》2019,39(1):117-128

尘卷风是近地面气层中的小旋风,使沙尘或其他细小物体随风卷起而形成的一种天气现象。2011年10月27日11时10分和2015年9月13日11时12分发生于上海地区的两次强尘卷风天气过程(北京时,下同)均造成了不同程度的灾害。两次尘卷风均发生在温室大棚区,其下垫面性质和干旱区裸露地面和水泥沥青城市地面极不相同,因此了解其发生原因很有必要。本文利用常规天气图、温度对数压力图、100 m以下5层铁塔风和温度、微波辐射仪以及温室大棚基地自动气象站等资料对这两次尘卷风过程进行了分析。发现.在常规探空都未探测到明显的超绝热现象,但在铁塔观测的地表面层温度垂直廓线结合微波辐射仪及自动气象站等资料揭示了尘卷风发生时近地面气层都具备了超绝热条件。尘卷风发生前后10∶00—12∶00的10～70 m温度垂直递减率γ平均达1.58℃/100 m,极大值达2.33℃/100 m,为干绝热递减率的两倍还多。上海地区10座铁塔测风网获得的10、30、50、70 m近地层风场的旋转和辐合特征揭示了尘卷风旋转的角动量来源。通过分析500、700、850 hPa天气形势探讨了有利于发生尘卷风的大尺度环流条件为尘卷风预报提供参考。最后对这两次尘卷风发生在温室大棚区域而不是自然农田的机理提出了初步看法供进一步讨论。  相似文献   

阵风因子与大气边界层要素的关系及预报试验     

胡波 《气象科技》2019,47(2):282-288

利用2008—2016年舟山4个海岛气象站大风资料和欧洲中心的ERA-interim再分析资料,分析了阵风因子随平均风速、风向、小时、月份等分布的气候特征,统计阵风因子与边界层的大气稳定度、250～1000m风速与10m风速的比值、6h变温等要素的相关后,选取最佳预报因子,利用BP人工神经网络方法,根据不同因子组合对阵风进行循环试报。结果表明:①平均风速较小时阵风因子波动范围大;靠近大陆站点的阵风因子及来自陆地方向气流的阵风因子偏大。②白天11:00—16:00受太阳辐射影响大气湍流相对较强,阵风因子偏大。7—9月沿海受台风影响频繁,其阵风因子要大些,而11—12月阵风因子偏大则与来流方向的地表粗糙度较大有关。③阵风因子和边界层不同高度的风速与10m风速比值,及气温具有明显正相关,与边界层大气稳定度参数具有负相关,相关结果印证了阵风主要物理成因与动量的垂直湍流输送有关。④阵风循环试报表明最佳组模型试报的绝对误差及方差均比对比组模型减少约11%～25%,具有较好的预报效果。  相似文献   

Multifractal Characteristics of Intermittent Turbulence in the Urban Canopy Layer          下载免费PDF全文

XU Jing-Jing  HU Fei 《大气和海洋科学快报》2015,8(2):72-77

The multifractality of energy and thermal dissipation of fully developed intermittent turbulence is investigated in the urban canopy layer under unstable conditions by the singularity spectrum for the fractal dimensions of sets of singularities characterizing multifractals. In order to obtain high-order moment properties of smallscale turbulent dissipation in the inertial range, an ultrasonic anemometer with a high sampling frequency of 100 Hz was used. The authors found that the turbulent signal could be singular everywhere. Moreover, the singular exponents of energy and thermal dissipation rates are most frequently encountered at around 0.2, which is significantly smaller than the singular exponents for a wind tunnel at a moderate Reynolds number. The evidence indicates a higher intermittency of turbulence in the urban canopy layer at a high Reynolds number, which is demonstrated by the data with high temporal resolution. Furthermore, the temperature field is more intermittent than the velocity field. In addition, a large amount of samples could be used for verification of the results.  相似文献   

Analysis of atmospheric turbulence in the upper layers of sea fog     

李永平  郑运霞 《中国海洋湖沼学报》2015,33(3):809-818

Atmospheric turbulence plays a vital role in the formation and dissipation of fog. However,studies of such turbulence are typically limited to observations with ultrasonic anemometers less than 100 m above ground. Thus,the turbulence characteristics of upper fog layers are poorly known. In this paper,we present 4-layers of data,measured by ultrasonic anemometers on a wind tower about 400 m above the sea surface; we use these data to characterize atmospheric turbulence atop a heavy sea fog. Large differences in turbulence during the sea fog episode were recorded. Results showed that the kinetic energy,momentum flux,and sensible heat flux of turbulence increased rapidly during the onset of fog. After onset,high turbulence was observed within the uppermost fog layer. As long as this turbulence did not exceed a critical threshold,it was crucial to enhancing the cooling rate,and maintaining the fog. Vertical momentum flux and sensible heat flux generated by this turbulence weakened wind speed and decreased air temperature during the fog. Towards the end of the fog episode,the vertical distribution of sensible heat flux reversed,contributing to a downward momentum flux in all upper layers. Spatial and temporal scales of the turbulence eddy were greater before and after the fog,than during the fog episode. Turbulence energy was greatest in upper levels,around 430 m and 450 m above mean sea level(AMSL),than in lower levels of the fog(390 m and 410 m AMSL); turbulence energy peaked along the mean wind direction. Our results show that the status of turbulence was complicated within the fog; turbulence caused fluxes of momentum and sensible heat atop the fog layer,affecting the underlying fog by decreasing or increasing average wind speed,as well as promoting or demoting air temperature stratification.  相似文献   

A mobile polar atmospheric parameter measurement system:II. First atmospheric turbulence observation at Antarctic Taishan Station     

TIAN Qiguo  JIANG Peng  WU Xiaoqing  JIN Xinmiao  LU Shan  JI Tuo  CHAI Bo  ZHANG Shaohua  ZHOU Hongyan 《极地研究(英文版)》2015,(2)

This is the second paper of a series devoted to atmospheric optical turbulence Cn2 observation using a mobile polar atmospheric parameter measurement system. We present the initial results of Cn2 measu...  相似文献   

On the maximal value of the turbulent α ‐parameter in accretion discs     

P. Abolmasov  N.I. Shakura 《Astronomische Nachrichten》2009,330(7):737-740

In this short paper we show that making turbulence two‐rather than three‐dimensional may increase the effective turbulent viscosity by about 40 %. Dimensionless hydrodynamical viscosity parameters up to α_max = 0.25 M_t² may be obtained in this approach, which are in better agreement with the observational data on non‐stationary accretion than the values obtained in numerical simulations. However, the α ‐parameter values known from observations are still several times higher (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Mean-field effects in the Galloway–Proctor flow     

Karl-Heinz Rädler  Axel Brandenburg 《Monthly notices of the Royal Astronomical Society》2009,393(1):113-125

In the framework of mean-field electrodynamics the coefficients defining the mean electromotive force in Galloway–Proctor flows are determined. These flows show a two-dimensional pattern and are helical. The pattern wobbles in its plane. Apart from one exception a circularly polarized Galloway–Proctor flow, i.e. a circular motion of the flow pattern is assumed. This corresponds to one of the cases considered recently by Courvoisier, Hughes & Tobias. An analytic theory of the α effect and related effects in this flow is developed within the second-order correlation approximation and a corresponding fourth-order approximation. In the validity range of these approximations there is an α effect but no γ effect, or pumping effect. Numerical results obtained with the test-field method, which are independent of these approximations, confirm the results for α and show that γ is in general non-zero. Both α and γ show a complex dependency on the magnetic Reynolds number and other parameters that define the flow, that is, amplitude and frequency of the circular motion. Some results for the magnetic diffusivity  η_t  and a related quantity are given, too. Finally, a result for α in the case of a randomly varying linearly polarized Galloway–Proctor flow, without the aforementioned circular motion, is presented. The flows investigated show quite interesting effects. There is, however, no straightforward way to relate these flows to turbulence and to use them for studying properties of the α effect and associated effects under realistic conditions.  相似文献   

Kolmogorov dissipation scales in weakly ionized plasmas     

V. Krishan  Z. Yoshida 《Monthly notices of the Royal Astronomical Society》2009,395(4):2039-2044

In a weakly ionized plasma, the evolution of the magnetic field is described by a 'generalized Ohm's law' that includes the Hall effect and the ambipolar diffusion terms. These terms introduce additional spatial and time-scales which play a decisive role in the cascading and the dissipation mechanisms in magnetohydrodynamic turbulence. We determine the Kolmogorov dissipation scales for the viscous, the resistive and the ambipolar dissipation mechanisms. The plasma, depending on its properties and the energy injection rate, may preferentially select one of these dissipation scales, thus determining the shortest spatial scale of the supposedly self-similar spectral distribution of the magnetic field. The results are illustrated taking the partially ionized part of the solar atmosphere as an example. Thus, the shortest spatial scale of the supposedly self-similar spectral distribution of the solar magnetic field is determined by any of the four dissipation scales given by the viscosity, the Spitzer resistivity (electron–ion collisions), the resistivity due to electron–neutral collisions and the ambipolar diffusivity. It is found that the ambipolar diffusion dominates for reasonably large energy injection rate. The robustness of the magnetic helicity in the partially ionized solar atmosphere would facilitate the formation of self-organized vortical structures.  相似文献   

A study of interstellar medium of dwarf galaxies using H i power spectrum analysis     

Prasun Dutta  Ayesha Begum  Somnath Bharadwaj  Jayaram N. Chengalur 《Monthly notices of the Royal Astronomical Society》2009,398(2):887-897

We estimate the power spectrum of H  i intensity fluctuations for a sample of eight galaxies (seven dwarf and one spiral). The power spectrum can be fitted to a power-law     for six of these galaxies, indicating turbulence is operational. The estimated best-fitting value for the slope ranges from  ∼−1.5  (AND IV, NGC 628, UGC 4459 and GR 8) to  ∼−2.6  (DDO 210 and NGC 3741). We interpret this bi-modality as being due to having effectively 2D turbulence on length-scales much larger than the scale-height of the galaxy disc and 3D otherwise. This allows us to use the estimated slope to set bounds on the scale-heights of the face-on galaxies in our sample. We also find that the power-law slope remains constant as we increase the channel thickness for all these galaxies, suggesting that the fluctuations in H  i intensity are due to density fluctuations and not velocity fluctuations, or that the slope of the velocity structure function is ∼0. Finally, for the four galaxies with '2D turbulence' we find that the slope α correlates with the star formation rate (SFR) per unit area, with larger SFRs leading to steeper power laws. Given our small sample size, this result needs to be confirmed with a larger sample.  相似文献   

The role of the Yoshizawa effect in the Archontis dynamo     

Sharanya Sur  Axel Brandenburg 《Monthly notices of the Royal Astronomical Society》2009,399(1):273-280

The generation of mean magnetic fields is studied for a simple non-helical flow where a net cross-helicity of either sign can emerge. This flow, which is also known as the Archontis flow, is a generalization of the Arnold–Beltrami–Childress flow, but with the cosine terms omitted. The presence of cross-helicity leads to a mean-field dynamo effect that is known as the Yoshizawa effect. Direct numerical simulations of such flows demonstrate the presence of magnetic fields on scales larger than the scale of the flow. Contrary to earlier expectations, the Yoshizawa effect is found to be proportional to the mean magnetic field and can therefore lead to its exponential instead of just linear amplification for magnetic Reynolds numbers that exceed a certain critical value. Unlike α effect dynamos, it is found that the Yoshizawa effect is not notably constrained by the presence of a conservation law. It is argued that this is due to the presence of a forcing term in the momentum equation, which leads to a non-zero correlation with the magnetic field. Finally, the application to energy convergence in solar wind turbulence is discussed.  相似文献