《内蒙古气象》来稿中常见问题分析     

任晓萌 《内蒙古气象》2011,(6):104-105,118

针对目前科技论文写作出现的问题,选取了《内蒙古气象》2010年第6期到2011年第5期共121篇论文,主要采用记录和统计手段对来稿出现的常见问题进行了分析。分析结果显示,论文写作存在的问题主要集中在论文撰写格式和规范化程度、叙述的合理性、推理的逻辑性、写作的条理性和表达的准确性等方面。  相似文献   

气象-气溶胶资料联合同化对秋季PM_2.5浓度模拟的影响研究     

宋佳琨  陈耀登  陈丹 《气象学报》2021,79(3):477-491

相比冬季大范围静稳条件下的污染堆积过程,秋季气象条件更加复杂和局地化,气象条件模拟不确定性给秋季气溶胶模拟带来了更大难度,且目前研究较少考虑气象-气溶胶因素在线模拟和联合同化。使用WRF/Chem模式和格点统计差值（GSI）三维变分同化系统,2015年10月进行了为期1个月的气象-气溶胶资料联合同化及模拟试验,并基于此讨论了气象-气溶胶资料联合同化对秋季PM_2.5浓度模拟的影响。结果表明,WRF/Chem模式可以模拟出秋季污染天气过程,但对华北平原和中东部地区存在高估、西北部存在低估现象;同化地面PM_2.5浓度观测资料可以改进对PM_2.5浓度的模拟,上述两个地区的偏差均得到订正,6 h预报偏差均降低至6 μg/m3以内;重点针对华北地区的分析表明,秋季PM_2.5污染过程与特殊气象条件（湿度升高、风场辐合、区域输送）密切相关,因此在地面PM_2.5观测资料同化基础上增加常规气象资料同化,能进一步提高对华北平原气象-污染过程的表达,PM_2.5浓度预报相关系数从0.86提高至0.89。气象-气溶胶联合资料同化能更加准确地模拟秋季气溶胶污染过程,为更好地开展污染成因和在气象预报框架下开展气象-气溶胶相互影响研究提供了基础。   相似文献   

COVID-19疫情期间全球空气质量变化:臭氧响应的区域间差异          下载免费PDF全文

Rong Tang  Xin Huang  Derong Zhou  Haikun Wang  Jiawei Xu  Aijun Ding 《大气和海洋科学快报》2021,14(4):45-51

疫情期间全球各地一次排放大幅削减,而臭氧等二次污染的响应则存在着区域间差异.结合地面和卫星观测发现,同在氮氧化物大幅下降的情况下,臭氧在东亚和欧洲呈现出可达14ppb的上升信号,而北美则下降为主(约2-4ppb).我们结合气象分析和臭氧敏感性进一步讨论了臭氧响应差异性的原因,一方面受臭氧与前体物间关系的影响;另一方面来自于气象,尤其是温度.研究明晰了人为排放,化学和气象三者的内在关联,强调了在臭氧控制过程中考虑前体物削减和气象条件协同的重要性.  相似文献   

Assimilation of thermal emission spectrometer atmospheric data during the Mars Global Surveyor aerobraking period     

Stephen R. Lewis  Peter L. Read  Barney J. Conrath  John C. Pearl  Michael D. Smith 《Icarus》2007,192(2):327-347

The Thermal Emission Spectrometer aboard the Mars Global Surveyor spacecraft has produced an extensive atmospheric data set, beginning during aerobraking and continuing throughout the extended scientific mapping phase. Temperature profiles for the atmosphere below about 40 km, surface temperatures and total dust and water ice opacities, can be retrieved from infrared spectra in nadir viewing mode. This paper describes assimilation of nadir retrievals from the spacecraft aerobraking period, L_S=190°–260°, northern hemisphere autumn to winter, into a Mars general circulation model. The assimilation scheme is able to combine information from temperature and dust optical depth retrievals, making use of a model forecast containing information from the assimilation of earlier observations, to obtain a global, time-dependent analysis. Given sufficient temperature retrievals, the assimilation procedure indicates errors in the a priori dust distribution assumptions even when lacking dust observations; in this case there are relatively cold regions above the poles compared to a model which assumes a horizontally-uniform dust distribution. One major reason for using assimilation techniques is in order to investigate the transient wave behavior on Mars. Whilst the data from the 2-h spacecraft mapping orbit phase is much more suitable for assimilation, even the longer (45–24 h) period aerobraking orbit data contain useful information about the three-dimensional synoptic-scale martian circulation which the assimilation procedure can reconstruct in a consistent way. Assimilations from the period of the Noachis regional dust storm demonstrate that the combined assimilation of temperature and dust retrievals has a beneficial impact on the atmospheric analysis.  相似文献   

非线性层结与对流运动的稳定性     

陈忠明 《成都信息工程学院学报》1991,(Z1)

本文讨论了温度层结为普遍化三次分布情况下对流运动的分岔和突变特征,得到了一些有意义的结果,加深了我们对非线性对流运动特征的一些认识。  相似文献   

静力平衡近似下大气中非线性对称运动的稳定性、分岔和突变     

彭晓林  罗德海 《成都信息工程学院学报》1991,(Z1)

本文在考虑基本气流具有非线性切变情况下,导出了对称运动所满足的非线性常微分方程,并用非线性系统的稳定、分岔、突变理论,严格地讨论了非线性对称运动的稳定性、分岔和突变问题,获得了一个推广的对称不稳定判据,找到了突变产生的条件。  相似文献   

青藏高原500hpa暖性高压生成的热成风适应机制     

李国平  万军  邓思华 《成都信息工程学院学报》1991,(Z1)

本文利用热成风适应原理,采取分解分析法对青藏高原500hpa暖性高压的生成机制作了一些定性和定量的讨论。结果表明:在扰动的水平尺度大于热成风适应的特征尺度的条件下,当源地有明显的负值非热成风涡度出现时,流场将向温度场适应,而温度场由于高原的加热作用存在暖中心或暖脊,则适应的结果在高原大气500hpa形成暖性高压,并伴随高层辐合,低层辐散及下沉运动。  相似文献   

Thermal interactions of the Huygens probe with the Titan environment: Constraint on near-surface wind     

Ralph D. Lorenz 《Icarus》2006,182(2):559-566

The Huygens probe lost heat to its cold environment during its descent through Titan's atmosphere and after landing. Here I report measurements of the probe's thermal behavior and comparison with ground tests (1) to provide a context for other scientific investigations, such as the release of volatiles from the landing site, and (2) to place constraints on Titan environmental parameters directly, such as the thermal conductivity of the surface material and the strength of winds at the surface. Near-surface winds are constrained to be less than 0.2 m s⁻¹, and probably much less.  相似文献   

Meteorological assessment of the surface temperatures on Titan: constraints on the surface type     

Tetsuya Tokano 《Icarus》2005,173(1):222-242

The latitudinal profile of near-surface air temperature on Titan retrieved by Voyager 1 has been difficult to understand and raised several speculations about possible exotic processes that might be occurring near Titan's surface, while the thermal properties of the surface itself are unknown. This study systematically investigates the seasonal and spatial variation of the surface temperature and air temperature in the lower troposphere by a 3-dimensional general circulation model for different putative surface types (porous icy regolith, rock-ice mixture, hydrocarbon lakes). For any viable surface type the surface temperature is unlikely to be constant through the year and should more or less vary seasonally and even diurnally, most likely by a few K. Recent observations of tropospheric clouds may be evidence of seasonal variation of the surface temperature and the model predicts in the case of solid surface the development of a convective layer with superadiabatic lapse rates near the surface exactly at those latitudes and seasons where clouds have been identified. The latitudinal profile of the surface temperature retrieved from Voyager 1 infrared spectra can be explained without invoking exotic effects, provided the thermal inertia of the surface is relatively small and/or the surface albedo is low. A dominance of water ice (high thermal inertia and high albedo) at the surface is unfavorable to reproduce the observation. The latitudinal gradient of the surface temperature is particularly large at the hydrocarbon lake surface due to low albedo and small surface drag. Local anomalies of the surface albedo or surface thermal inertia are likely to cause substantial inhomogeneities of the surface temperature. Quasi-permanent accumulation of stratospheric haze at both poles would create a perennial equator-to-pole contrast of the surface temperature, but also a substantially lower global-mean surface temperature due to an enhanced anti-greenhouse effect in summer. The air temperature in the lower troposphere exhibits a tiny latitudinal gradient and a pole-to-pole gradient due to the presence of a pole-to-pole Hadley circulation, indicating that the temperature within the planetary boundary layer may exhibit a vertical profile characteristic of season, location and scenario. There may be a shallow near-surface inversion layer in cold seasons and a shallow convective layer in warm seasons.  相似文献   

A three-dimensional model of moist convection for the giant planets II: Saturn's water and ammonia moist convective storms     

Ricardo Hueso  Agustín Sánchez-Lavega 《Icarus》2004,172(1):255-271

Moist convective storms constitute a key aspect in the global energy budget of the atmospheres of the giant planets. Among them, Saturn is known to develop the largest scale convective storms in the Solar System, the Great White Spots (GWS) which occur rarely and have been detected once every 30 years approximately. On the average, Saturn seems to show much less convective storms than Jupiter with smaller size and reduced frequency and intensity. Here we present detailed simulations of the onset and development of storms at the Equator and mid-latitudes of Saturn. These are the regions where most of the recent convective activity of the planet has been observed. We use a 3D anelastic model with parameterized microphysics (Hueso and Sánchez-Lavega, 2001, Icarus 151, 257) studying the onset and evolution of water and ammonia moist convective storms up to sizes of a few hundred km. Water storms, while more difficult to initiate than in Jupiter, can be very energetic, arriving to the 150 mbar level and developing vertical velocities on the order of 150 m s⁻¹. Ammonia storms develop easier but with a much smaller intensity unless very large abundances of ammonia (10 times solar) are present in Saturn's atmosphere. The Coriolis forces play a major role in the morphology and properties of water based storms.  相似文献