复杂下垫面模拟域大气边界层非局地闭合模拟研究

在非局地闭合大气边界层模拟研究基础上,选取黑河实验研究资料（HEIFE）,利用二维模式对绿洲和沙漠交界地区的内边界层结构进行了模拟研究,模式考虑了两种下垫面条件下动力、热力特性的不同,并加入了湿度及水汽通量的预报。模拟结果表明:二维非局地闭合模式能得到合理的TIBL结构的基本特征,包括平均场、湍流场等,并能模拟给出一些由下垫面特性形成的大气现象,如沙漠地区逆湿现象的生消过程、绿洲的冷岛效应、绿洲与沙漠因热力差异而形成的局部环流形势等细致结构,符合沙漠站白天观测事实的典型特征。     

BJ-RUC系统对北京夏季边界层的预报性能评估

以北京市观象台2010年8月、2011年8月每日3次 (08:00, 14:00, 20:00,北京时,下同) L波段探空秒间隔数据为实况,对BJ-RUC系统 (rapid updated cycle system for the Beijing area) 分析和预报边界层性能进行了初步评估。结果表明:BJ-RUC系统对北京地区夏季白天边界层的细致特征具有较好的预报能力,但也存在明显的系统性误差。08:00边界层偏冷; 14:00和20:00 1 km以下的边界层则显著偏暖, 边界层内明显偏湿。整体上模式对边界层内温度、湿度的预报误差均高于自由大气。该系统对北京地区边界层内早晨 (08:00) 从夜间山风向白天谷风环流过渡、午后 (14:00) 到日落后 (20:00)1500 m以下盛行西南偏南气流的日变化特征具有较强的预报能力。系统预报的14:00边界层顶高度与评估时段内实际对流边界层高度的变化趋势一致。但预报的对流边界层顶偏高,这与BJ-RUC系统采用YSU边界层参数化方案的垂直混合更强有关。     

On the unmodeled perturbations in the motion of uranus

In this paper we apply a numerical method to determine unmodeled perturbations in an attempt to explain the observed discrepancies in the motion of Uranus. We find that the estimated perturbation shows some significant periods that could be attributed to insufficient knowledge of the perturbations from some of the known planets. On the assumption that the gravitational attraction of an unknown planet is the origin of the deviations, the best planar solution of the inverse problem is a planet of 0.6 Earth masses, with true longitude of 133° (1990.5), semi major axis a = 44 AU and eccentricity e = 0.007.     

北半球冬季行星波的传播及其输运作用

利用变换欧拉平均方程讨论了行星波动力学。观测和模拟结果都表明,在北半球冬季准定常行星波的经向传播存在两支波导。一支为高纬度波导,另一支则为低纬度波导。这些结果与理论分析相当一致。通过对EP通量进一步的研究表明,平流层爆发性增温是沿高纬度波导传播的异常行星波与平均气流相互作用的结果。而热带风场的准两年周期振荡（QBO）是低纬度平流层下层大气纬向平均流的一个重要年际变化,它可以影响行星波沿低纬度波导的传播;此外,由一个行星波一平均流耦合模式模拟的结果表明,这个热带风场的变化还可以通过波流相互作用调制行星波沿高纬度波导的传播。 行星波对臭氧的输运作用在文中也进行了分析。行星波强迫出的剩余平均环流表明,耗散的行星波有强的输运作用;向北的涡动热量输送可以强迫出一个正的输运环流,其在低纬度上升并在高纬度下沉。同时研究还表明,热带风场的QBO对行星波传播的调制对输运环流也有重要影响,模式结果表明,在QBO的东风位相期间行星波引起的输运作用明显增强,其结果可用于解释平流层高纬度臭氧的年际变化。     

边界层方案对一次西南涡背景下局地暴雨过程影响分析北大核心

利用WRF模式对2017年6月9日重庆合川区一次局地暴雨过程开展对流可分辨尺度的模拟试验,比较三种边界层参数化方案对降水模拟的影响。结果表明,不同试验均能模拟出此次降水的主要分布特征,而不同边界层参数化方案能够显著影响降水落区和强度的模拟。MYJ方案对强降水的模拟最好,能较好地模拟出降水触发的时间和位置;其次为BouLac方案,触发时间偏晚约2 h,降水落区与MYJ方案相近;YSU方案模拟的降水分布偏差较大,降水触发的位置和落区偏北。湍流混合强度是造成落区模拟差异的主要原因,通过影响1.5 km高度以下风场分布改变造成此次局地强降水过程的西南涡位置,进而影响到降水的落区。基于YSU方案的湍流混合减弱试验证明了湍流混合强度与降水落区的关系。     

Study of resonances for the restricted 3‐body problem

Our aim is to identify and classify mean‐motion resonances (MMRs) for the coplanar circular restricted three‐body problem (CR3BP) for mass ratios between 0.10 and 0.50. Our methods include the maximum Lyapunov exponent, which is used as an indicator for the location of the resonances, the Fast Fourier Transform (FFT) used for determining what kind of resonances are present, and the inspection of the orbital elements to classify the periodicity. We show that the 2:1 resonance occurs the most frequently. Among other resonances, the 3:1 resonance is the second most common, and furthermore both 3:2 and 5:3 resonances occur more often than the 4:1 resonance. Moreover, the resonances in the coplanar CR3BP are classified based on the behaviour of the orbits. We show that orbital stability is ensured for high values of resonance (i.e., high ratios) where only a single resonance is present. The resonances attained are consistent with the previously established resonances for the solar system, i.e., specifically, in regards to the asteroid belt. Previous work employed digital filtering and Lyapunov characteristic exponents to determine stochasticity of the eccentricity, which is found to be consistent with our usage of Lyapunov exponents as an alternate approach based on varying the mass ratio instead of the eccentricity. Our results are expected to be of principal interest to future studies, including augmentations to observed or proposed resonances, of extra‐solar planets in binary stellar systems (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The 2200 Å bump and the interstellar extinction curve

The 2200 Å bump is a major figure of interstellar extinction. However, extinction curves with no bump exist and are, with no exception, linear from the near‐infrared down to 2500 Å at least, often over all the visible‐UV spectrum. The duality linear versus bump‐like extinction curves can be used to re‐investigate the relationship between the bump and the continuum of interstellar extinction, and answer questions as why do we observe two different kinds of extinction (linear or with a bump) in interstellar clouds? How are they related? How does the existence of two different extinction laws fits with the requirement that extinction curves depend exclusively on the reddening E (B – V) and on a single additional parameter? What is this free parameter? It will be found that (1) interstellar dust models, which suppose the existence of three different types of particles, each contributing to the extinction in a specific wavelength range, fail to account for the observations; (2) the 2200 Å bump is very unlikely to be absorption by some yet unidentified molecule; (3) the true law of interstellar extinction must be linear from the visible to the far‐UV, and is the same for all directions including other galaxies (as the Magellanic Clouds). In extinction curves with a bump the excess of starlight (or the lack of extinction) observed at wavelengths less than λ = 4000 Å arises from a large contribution of light scattered by hydrogen on the line of sight. Although counter‐intuitive this contribution is predicted by theory. The free parameter of interstellar extinction is related to distances between the observer, the cloud on the line of sight, and the star behind it (the parameter is likely to be the ratio of the distances from the cloud to the star and to the observer). The continuum of the extinction curve and the bump contain no information on the chemical composition of interstellar clouds. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

High‐resolution simulations and visualization of protoplanetary disks: structure of the flow in the vicinity of a massive planet

A problem of mass flow in the immediate vicinity of a planet embedded in a protoplanetary disk is studied numerically in two dimensions. Large differences in temporal and spatial scales involved suggest that a specialized discretization method for solution of hydrodynamical equations may offer great savings in computational resources, and can make extensive parameter studies feasible. Preliminary results obtained with help of Adaptive Mesh Refinement technique and high‐order explicit Eulerian solver are presented. This combination of numerical techniques appears to be an excellent tool which allows for direct simulations of mass flow in vicinity of the accretor at moderate computational cost. The present communication is focused on the structure of the outer part of the circumplanetary disk. We employ the multifluid option to the hydrodynamical solver to prove that the circumplanetary disk is composed of the gas transfered into it from the edges of the gap.     

Spectroscopic verification of suspected planetary nebulae. IV.

Verification of 7 objects as PNe (Table 1/A) as well as misclassification of 5 objects as PNe (Table 1/C) are discussed according to our CCD spectra; the status of 4 objects (Table 1/B) remains uncertain. In Table we give the estimates of line‐strengths and the measured intensities of emission lines as well as the derived hel. radial velocities and their standard deviations.