高原东侧特大暴雨过程中秦岭山脉的作用   总被引：8，自引：5，他引：3       下载免费PDF全文

慕建利  李泽椿  李耀辉 《高原气象》2009,28(6):1282-1290

利用中尺度数值模式MM5V3.5对2002年6月8～9日陕西特大暴雨过程进行了数值模拟, 在模拟结果和实况较吻合的情况下, 通过敏感性试验, 研究了秦岭山脉在这次暴雨过程中所起的作用。结果表明, 秦岭山脉在这次暴雨过程中对降水的强度有很大的影响, 即秦岭山脉使陕甘宁边界的长城沿线、 秦岭山脉、 汉江河谷一带降水量增加, 使关中盆地、 陕北南部、 大巴山东南坡降水量减少。进一步研究表明, 秦岭山脉主要是通过形成局地环流, 使气流产生辐合, 大量的水汽和位势不稳定能量在迎风坡堆积, 上升运动加强, 从而使位势不稳定能量得以释放, 触发了对流降水。  相似文献   

北京夏季日最大电力负荷预报模型建立方法探讨   总被引：2，自引：1，他引：1  

叶殿秀  张培群  赵珊珊  夏鑫  柯宗建  王有民  刘秋锋 《气候与环境研究》2013,18(6):804-810

为了探索夏季(6～8月)日气象负荷的最佳分离方式和引起日最大电力负荷波动的主要因子,以及建立预报模型最佳个数,基于北京市2005～2010年逐日最大电力负荷和同期的气象资料,分析了北京地区日最大电力负荷的变化规律,采用不同方法将气象负荷从夏季日最大电力负荷中分离出来,分析北京夏季气象负荷与气温、相对湿度、降水及炎热指数、高温持续日数、炎热日数持续时间、前一日气象负荷等因子之间的关系,并基于2005～2009年夏季逐日气象负荷和其主要影响因子采用逐步回归方法建立日最大电力负荷的预报模型,将2010年夏季北京日最大电力负荷作为预报效果的独立样本检验。结果显示:2005～2010年,北京逐日最大电力负荷具有明显的线性增长趋势,夏季日最大电力负荷具有显著的星期效应;与去掉逐年夏季日最大电力负荷趋势和夏季平均日最大电力负荷趋势相比,去掉全年逐日最大电力负荷变化趋势的夏季日气象负荷预报模型的拟合能力更优;北京夏季日气象负荷与当日气温的相关系数最高,与前一日气象负荷也关系密切;利用前一日相对气象负荷和当日气象要素一周逐日分别建立预报模型的拟合和预测效果较好。  相似文献   

深圳市高影响天气的风廓线雷达特征   总被引：1，自引：0，他引：1  

陈元昭  彭勇刚  王明洁  陈训来 《广东气象》2010,32(3):12-16

利用深圳多年风廓线雷达观测资料,分析了灰霾、大雾、高温、雷暴、台风、冷空气等高影响天气过程中的风廓线特征。结果表明风廓线雷达作为一种新型的探测工具,能够在垂直方向获取较高时间、空间分辨率的实时资料,为分析、预报预警高影响天气提供了新的资料和观测事实。不同的高影响天气风廓线特征各不相同。灰霾和高温以上空出现东北风为特征:大雾的水平、垂直方向分布与信噪比有关;雷暴等强对流天气具有明显的风垂直切变;热带气旋、西风槽和锋面等移动性天气系统,其风向、风速的垂直分布随时间有明显变化。  相似文献   

西北干旱区夏半年深厚的混合层与干旱气候形成   总被引：8，自引：3，他引：5       下载免费PDF全文

李岩瑛  钱正安  薛新玲  兰晓波  李玲萍 《高原气象》2009,28(1):46-54

为了更好地理解西北干旱区大气混合层(ML)厚度的变化特征及其对当地干旱气候形成的影响,我们利用张掖和民勤站夏季及相关月的实测探空资料及T-log P图解法,首先计算了该两地逐日ML厚度,然后分析并讨论了它的时空间变化特征、与干湿天气气候的关系,以及夏半年的深厚ML,对加剧当地干旱气候的影响.结果表明:(1)河西中东部ML厚度的年变化及地区差异明显.冬季最浅薄,夏半年深厚(特别是5、6月),4月及10月分别是ML急剧增厚及变薄的过渡期;同时,更靠近西北干旱区中心的河西西部及北部的ML更深厚.(2)夏季干(湿)天气通过加强(减弱)地气间的感热交换和干对流,而明显影响当地的ML厚度.平均而言,以高温日最深厚,千日次之,小雨日再次之,而中强雨日最浅薄.千年夏季的ML厚度平均比湿年的对应值增厚300 m左右.夏季典型千日的ML厚度比雨日厚3000 m,典型干日的ML厚度昼宿变化不大.(3)反过来夏半年深厚的ML也通过增加雨滴蒸发损耗,减少了干旱区的降水,加剧了当地干旱的程度,因此夏半年深厚的ML也是形成干旱气候背景的成因之一.  相似文献   

Spectral properties of simulated impact glasses produced from martian soil analogue JSC Mars-1     

L.V. Moroz  A.T. Basilevsky  S.S. Rout  C.H. van der Bogert  A.V. Fisenko  V.S. Rusakov  N.G. Zinovieva  C.M. Pieters 《Icarus》2009,202(1):336-353

To simulate the formation of impact glasses on Mars, an analogue of martian bright soil (altered volcanic soil JSC Mars-1) was melted at relevant oxygen fugacities using a pulsed laser and a resistance furnace. Reduction of Fe³⁺ to Fe²⁺ and in some cases formation of nanophase Fe⁰ in the glasses were documented by Mössbauer spectroscopy and TEM studies. Reflectance spectra for several size fractions of the JSC Mars-1 sample and the glasses were acquired between 0.3 and 25 μm. The glasses produced from the JSC Mars-1 soil show significant spectral variability depending on the method of production and the cooling rate. In general, they are dark and less red in the visible compared to the original JSC Mars-1 soil. Their spectra do not have absorption bands due to bound water and structural OH, have positive spectral slopes in the near-infrared range, and show two broad bands centered near 1.05 and 1.9 μm, typical of glasses rich in ferrous iron. The latter bands and low albedo partly mimic the spectral properties of martian dark regions, and may easily be confused with mafic materials containing olivine and low-Ca pyroxene. Due to their disordered structures and vesicular textures, the glasses show relatively weak absorption features from the visible to the thermal infrared. These weak absorption bands may be masked by the stronger bands of mafic minerals. Positive near-infrared spectral slopes typical of fresh iron-bearing impact or volcanic glasses may be masked either by oxide/dust coatings or by aerosols in the Mars' atmosphere. As a result, impact glasses may be present on the surface of Mars in significant quantities that have been either misidentified as other phases or masked by phases with stronger infrared features. Spectrometers with sufficient spatial resolution and wavelength coverage may detect impact glasses at certain locations, e.g., in the vicinity of fresh impact craters. Such dark materials are usually interpreted as accumulations of mafic volcanic sand, but the possibility of an impact melt origin of such materials also should be considered. In addition, our data suggest that high contents of feldspars or zeolites are not necessary to produce the transparency feature at 12.1 μm typical of martian dust spectra.  相似文献   

A survey of possible impact structures on 25143 Itokawa     

Naru Hirata  Olivier S. Barnouin-Jha  Chikatoshi Honda  Ryosuke Nakamura  Hideaki Miyamoto  Sho Sasaki  Hirohide Demura  Akiko M. Nakamura  Tatsuhiro Michikami  Robert W. Gaskell  Jun Saito 《Icarus》2009,200(2):486-502

We determined the morphologies and dimensions of possible impact craters on the surface of Asteroid 25143 Itokawa from images taken by the Hayabusa spacecraft. Circular depressions, circular features with flat floors or convex floors, and circular features with smooth surfaces were identified as possible craters. The survey identified 38 candidates with widely varying morphologies including rough, smooth and saddle-shaped floors, a lack of raised rims and fresh material exposures. The average depth/diameter ratio was 0.08±0.03: these craters are very shallow relative to craters observed on other asteroids. These shallow craters are a result of (1) target curvature influencing the cratering process, (2) raised rim not being generated by this process, and (3) fines infilling the craters. As many of the crater candidates have an unusual appearance, we used a classification scheme that reflects the likelihood of an observed candidate's formation by a hypervelocity impact. We considered a variety of alternative interpretations while developing this scheme, including inherited features from a proto-Itokawa, spall scars created by the disruption of the proto-Itokawa, spall scars following the formation of a large crater on Itokawa itself, and apparent depressions due to random arrangements of boulders. The size-frequency distribution of the crater candidates was close to the empirical saturation line at the largest diameter, and then decline with decreasing diameter.  相似文献   

Spin rates of fast-rotating asteroids and fragments in impact disruption     

Toshihiko Kadono  Masahiko Arakawa  Takashi Ito  Keiji Ohtsuki 《Icarus》2009,200(2):694-697

We present a new experimental result of fragment spin-rate in impact disruption, using a thin glass plate. A cylindrical projectile impacts on a side (edge) of the plate. Dispersed fragments are observed using a high-speed camera and the spin rates of fragments are measured. We find that the measured fragment spin-rate decreases with increasing size. Assuming that the rotational energy of fragments is supplied from the residual stress, the spin rate ω decreases with increasing fragment size r as ω∼r−1, which explains the above experimental results. This size-dependence is similar to that of the observed spin rates of small fast-rotating asteroids. Our results suggest that spin rates of fragments of small asteroids immediately after disruption may have a similar size-dependence, and can provide constraints on the subsequent spin-state evolution of small asteroids due to thermal torques.  相似文献   

Mass dispersal and angular momentum transfer during collisions between rubble-pile asteroids. II. Effects of initial rotation and spin-down through disruptive collisions     

Takaaki Takeda  Keiji Ohtsuki 《Icarus》2009,202(2):514-524

Expanding on our previous N-body simulation of impacts between initially non-rotating rubble-pile objects [Takeda, T., Ohtsuki, K., 2007. Icarus 189, 256-273], we examine effects of initial rotation of targets on mass dispersal and change of spin rates. Numerical results show that the collisional energy needed to disrupt a rubble-pile object is not sensitive to initial rotation of the target, in most of the parameter range studied in our simulations. We find that initial rotation of targets is slowed down through disruptive impacts for a wide range of parameters. The spin-down is caused by escape of high-velocity ejecta and asymmetric re-accumulation of fragments. When these effects are significant, rotation is slowed down even when the angular momentum added by an impactor is in the same direction as the initial rotation of the target. Spin-down is most efficient when the impact occurs in the equatorial plane of the target, because in this case most of the ejected fragments originate from the equatorial region of the target and a significant amount of angular momentum can be easily removed. In the case of impacts from directions inclined relative to the target's equatorial plane, spin-down still occurs with reduced degree, unless impacts occur onto the pole region from the vertical direction. Our results suggest that such spin-down through disruptive impacts may have played an important role in spin evolution of asteroids through collisions in the gravity-dominated regime.  相似文献   

Scaling of oblique impacts in frictional targets: Implications for crater size and formation mechanisms   总被引：1，自引：0，他引：1  

Dirk Elbeshausen  Kai Wünnemann 《Icarus》2009,204(2):716-731

Almost every meteorite impact occurs at an oblique angle of incidence, yet the effect of impact angle on crater size or formation mechanism is only poorly understood. This is, in large part, due to the difficulty of inferring impactor properties, such as size, velocity and trajectory, from observations of natural craters, and the expense and complexity of simulating oblique impacts using numerical models. Laboratory oblique impact experiments and previous numerical models have shown that the portion of the projectile’s kinetic energy that is involved in crater excavation decreases significantly with impact angle. However, a thorough quantification of planetary-scale oblique impact cratering does not exist and the effect of impact angle on crater size is not considered by current scaling laws. To address this gap in understanding, we developed iSALE-3D, a three-dimensional multi-rheology hydrocode, which is efficient enough to perform a large number of well-resolved oblique impact simulations within a reasonable time. Here we present the results of a comprehensive numerical study containing more than 200 three-dimensional hydrocode-simulations covering a broad range of projectile sizes, impact angles and friction coefficients. We show that existing scaling laws in principle describe oblique planetary-scale impact events at angles greater than 30° measured from horizontal. The displaced mass of a crater decreases with impact angle in a sinusoidal manner. However, our results indicate that the assumption that crater size scales with the vertical component of the impact velocity does not hold for materials with a friction coefficient significantly lower than 0.7 (sand). We found that increasing coefficients of friction result in smaller craters and a formation process more controlled by impactor momentum than by energy.  相似文献   

An empirical model for transient crater growth in granular targets based on direct observations     

Satoru Yamamoto  Olivier S. Barnouin-Jha  Seiji Sugita 《Icarus》2009,203(1):310-319

The present paper describes observations of crater growth up to the time of transient crater formation and presents a new empirical model for transient crater growth as a function of time. Polycarbonate projectiles were impacted vertically into soda-lime glass sphere targets using a single-stage light-gas gun. Using a new technique with a laser sheet illuminating the target [Barnouin-Jha, O.S., Yamamoto, S., Toriumi, T., Sugita, S., Matsui, T., 2007. Non-intrusive measurements of the crater growth. Icarus, 188, 506-521], we measured the temporal change in diameter of crater cavities (diameter growth). The rate of increase in diameter at early times follows a power law relation, but the data at later times (before the end of transient crater formation) deviates from the power law relation. In addition, the power law exponent at early times and the degree of deviation from a power law at later times depend on the target. In order to interpret these features, we proposed to modify Maxwell’s Z-model under the assumption that the strength of the excavation flow field decreases exponentially with time. We also derived a diameter growth model as: d(t)∝[1-exp(-βt)]^γ, where d(t) is the apparent diameter of the crater cavity at time t after impact, and β and γ are constants. We demonstrated that the diameter growth model could represent well the experimental data for various targets with different target material properties, such as porosity or angle of repose. We also investigated the diameter growth for a dry sand target, which has been used to formulate previous scaling relations. The obtained results showed that the dry sand target has larger degree of deviation from a power law, indicating that the target material properties of the dry sand target have a significant effect on diameter growth, especially at later times. This may suggest that the previously reported scaling relations should be reexamined in order to account for the late-stage behavior with the effect of target material properties.  相似文献