夏季青藏高原上的对流云和中尺度对流系统

运用1998年6～8月逐日逐时日本地球静止气象卫星(GMS)红外辐射亮温资料,计算和分析了青藏高原及周边地区对流云和中尺度对流系统的活动,揭示了它们形成和发展的月际变化和地理分布、强度、日变化、移动和传播等诸多特征,以及与长江流域暴雨过程的关系.     

Temporal evolution of MHD shocks in the interstellar medium

We undertake calculations of the time-dependent structure of shock waves propagating in dark and diffuse interstellar clouds. The results of the time-dependent model are compared with those obtained by means of an independent steady-state code and found to agree well at sufficiently late times. Discontinuities in the flow of the neutral fluid are handled by introducing a pseudo-viscosity. Special procedures are adopted to correct for the associated widening of the discontinuity, in order not to distort the role of inelastic collision processes. We find that, in dark clouds, C shocks will tend to predominate, but are unlikely to have attained steady state in the cloud lifetime. On the other hand, in diffuse clouds, steady state may be reached but the discontinuity in the flow of the neutral fluid remains. We find no evidence for the existence of C* shocks, in which the neutral fluid undergoes a continuous transition from supersonic to subsonic flow (in the reference frame of the shock wave). Attention is drawn to the possible importance of these results for the interpretation of H₂ rovibrational line intensities.     

A search for absorption of Mg and Ca compounds in molecular clouds towards Galactic continuum sources

Absorption lines of MgH and CaH N  = 1 − 0 transitions were searched for in foreground molecular clouds towards the continuum sources associated with Sgr B2 (M) and W49A (N). None of these lines was detected with our sensitivity level of ∼20 mK. Millimetric absorption lines of MgO, MgOH, CaO and CaOH were also searched for towards Sgr B2 (M) without success. The fractional abundances relative to molecular hydrogen are ≲ 1.0 × 10⁻¹¹ for MgH, ≲ 7.9 × 10⁻¹³ for MgO, ≲ 1.6 × 10⁻¹⁰ for MgOH, ≲ 1.6 × 10⁻⁹ for CaH, ≲ 2.0 × 10⁻¹² for CaO, and ≲ 2.5 × 10⁻¹⁰ for CaOH, respectively. The low abundances measured in absorption indicate that a significant fraction of interstellar magnesium and calcium cannot be tied up in their monohydrides, monoxides and monohydroxides. The low abundance of MgH also implies that grain-surface chemistry involving magnesium is not efficient and that magnesium is depleted on to grains to a factor of ≳ 10^2.5 in well-shielded molecular clouds.     

The size distribution of dust grains in single clouds – II. The analysis of extinction using inhomogeneous grains

The extinction curves of single clouds, seen towards the stars HD 147165, 179406 and 202904, have been modelled using various mixtures containing both the bare and inhomogeneous (composite and/or multilayer) grains. It has been shown that the models composed of the bare graphite and silicate grains together with the multilayer grains containing silicates, organic refractory and water ice, are more useful in explaining extinction under the reduced cosmic abundances. The models based on Mathis' composite grains or on Greenberg & Li's core-mantle grains can also provide quite good fits of the extinction and the measured scattering parameters, but still require an excessive amount of carbon which results in too large a C/O ratio. The inhomogeneous grains essentially contribute to the extinction in practically the whole wavelength range of our extinction curves. As a rule, such grains have quite wide size distributions, centred at around 100 nm, although graphite grains are mainly of small sizes.     

The interstellar clouds of adams and blaauw revisited: An HI absorption study-II

In the preceding paper (Paper I), we presented HI absorption spectra towards radio sources very close to the lines of sight towards twenty five bright stars against which optical absorption spectra had been obtained earlier, In this paper we analyse the results and draw some conclusions. To summarize briefly, in most cases we found HI absorption at velocities corresponding to the optical absorption features provided one restricted oneself to velocities ≲10 kms-1. At higher velocities we did not detect any HI absorption down to an optical depth limit of 0.1 (except in four cases which we attribute to gas in systematic motion rather than clouds in random motion). After discussing various scenarios, we suggest that this trend should perhaps be understood in terms of the high velocity interstellar clouds being accelerated, heated and ablated by expanding supernova remnants.     

The interstellar clouds of adams and blaauw revisited: An HI absorption study-I

This investigation is aimed at clarifying the nature of the interstellar gas seen in absorption against bright O and B stars. Towards this end we have obtained for the first time HI absorption spectra towards radio sources very close to the lines of sight towards twenty five bright stars previously studied. In this paper we describe the selection criteria, the details regarding our observations, and finally present the absorption spectra. In the accompanying paper we analyse the results and draw conclusions.     

Observations of nitric acid perturbations in the winter Arctic stratosphere: Evidence for PSC sedimentation

Gaseous nitric acid (HNO3) and hydrogene fluoride (HF) have been measured in the winter Arctic stratosphere using balloon- and aircraft-based Ion Molecule Reaction Mass Spectrometry (IMRMS) instruments. Strong HNO3 perturbations were found in 1993 and 1995 which may indicate nitrification around 11-13 km and denitrification around 20 km altitude. Most likely these perturbations were caused by sedimentation of HNO3 containing aerosols followed by aerosol evaporation at lower altitudes.     

车载LiDAR点云滤波的改进不规则三角网加密方法

针对当前城区车载LiDAR点云算法存在部分参数不易把握、需要多次人机交互、部分要素提取效果不好等问题,该文提出一种改进的TIN迭代加密滤波算法。首先,构建初始格网选取种子点,在选取种子点方面,采用邻域卷积和进行种子点的判断和虚拟种子点的构造;其次,进行TIN迭代加密滤波;最后根据滤波次数改变格网大小进行迭代滤波。采用SSW获取的北京城区某地点云数据进行试验,将实验结果与原始的TIN加密算法进行对比,并与其他两种滤波方法进行对比,结果表明,改进的方法能较好的适应城区情况,且能弥补其他方法的不足。