共查询到20条相似文献，搜索用时 843 毫秒
1.
In June 1985, two instrumented balloons were placed in the atmosphere of Venus as part of the VEGA mission. Each balloon traveled about 30 percent of the way around the planet at a float altitude near 54 kilometers. In situ sensors measured pressure, temperature, vertical wind velocity, cloud particle backscatter, ambient light level, and frequency of lightning. A ground-based network of 20 radio antennas tracked the balloons by very long baseline interferometry (VLBI) techniques to monitor the Venus winds. The history, organization, and principal characteristics of this international balloon experiment are described. 相似文献
2.
Linkin VM Kerzhanovich VV Lipatov AN Pichkadze KM Shurupov AA Terterashvili AV Ingersoli AP Crisp D Grossman AW Young RE Seiff A Ragent B Blamont JE Elson LS Preston RA 《Science (New York, N.Y.)》1986,231(4744):1417-1419
The VEGA balloons provided a long-term record of vertical wind fluctuations in a planetary atmosphere other than Earth's. The vertical winds were calculated from the observed displacement of the balloon relative to its equilibrium float altitude. The winds were intermittent; a large burst lasted several hours, and the peak velocity was 3 meters per second. 相似文献
3.
Linkin VM Kerzhanovich VV Lipatov AN Shurupov AA Seiff A Ragent B Young RE Ingersoll AP Crisp D Elson LS Preston RA Blamont JE 《Science (New York, N.Y.)》1986,231(4744):1420-1422
Thermal structure measurements obtained by the two VEGA balloons show the Venus middle cloud layer to be generally adiabatic. Temperatures measured by the two balloons at locations roughly symmetric about the equator differed by about 6.5 kelvins at a given pressure. The VEGA-2 temperatures were about 2.5 kelvins cooler and those of VEGA-1 about 4 kelvins warmer than temperatures measured by the Pioneer Venus Large Probe at these levels. Data taken by the VEGA-2 lander as it passed through the middle cloud agreed with those of the VEGA-2 balloon. Study of individual frames of the balloon data suggests the presence of multiple discrete air masses that are internally adiabatic but lie on slightly different adiabats. These adiabats, for a given balloon, can differ in temperature by as much as 1 kelvin at a given pressure. 相似文献
4.
Blamont JE Young RE Seiff A Ragent B Sagdeev R Linkin VM Kerzhanovich VV Ingersoll AP Crisp D Elson LS Preston RA Golitsyn GS Ivanov VN 《Science (New York, N.Y.)》1986,231(4744):1422-1425
Both VEGA balloons encountered vertical winds with typical velocities of 1 to 2 meters per second. These values are consistent with those estimated from mixing length theory of thermal convection. However, small-scale temperature fluctuations for each balloon were sometimes larger than predicted. The approximate 6.5-kelvin difference in temperature consistently seen between VEGA-1 and VEGA-2 is probably due to synoptic or planetary-scale nonaxisymmetric disturbances that propagate westward with respect to the planet. There is also evidence from Doppler data for the existence of solar-fixed nonaxisymmetric motions that may be thermal tides. Surface topography may influence atmospheric motions experienced by the VEGA-2 balloon. 相似文献
5.
6.
Seiff A Kirk DB Young RE Sommer SC Blanchard RC Findlay JT Kelly GM 《Science (New York, N.Y.)》1979,205(4401):46-49
The altitude profiles of temperature and pressure measured during the descent of the four Pioneer Venus probes show small contrast below the clouds but significant differences within the clouds at altitudes from 45 to 61 kilometers. At 60 kilometers, the probe which entered at 59.3 degrees north latitude sensed temperatures 25 K below those of the lower latitude probes, and a sizable difference persisted down to and slightly below the cloud base. It also sensed pressure below those of the other probes by as much as 49 millibars at a mean pressure of 200 millibars. The measured pressure differences are consistent with cyclostrophic balance of zonal winds ranging from 130 +/- 20 meters per second at 60 kilometers to 60 +/- 17 meters per second at 40 kilometers, with evidence in addition of a nonaxisymmetric component of the winds. The clouds were found to be 10 to 20 K warmer than the extended profiles of the lower atmosphere, and the middle cloud is convectively unstable. Both phenomena are attributed to the absorption of thermal radiation from below. Above the clouds, in the lower stratosphere, the lapse rate decreases abruptly to 3.5 K per kilometer, and a superimposed wave is evident. At 100 kilometers, the temperature is minimum, with a mean value of about 170 K. 相似文献
7.
Ingersoll AP 《Science (New York, N.Y.)》1990,248(4953):308-315
Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams. Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others. Large oval storm systems exhibit complicated time-dependent behavior that can be simulated in numerical models and laboratory experiments. The largest storm system, the Great Red Spot of Jupiter, has survived for more than 300 years in a chaotic shear zone where smaller structures appear and dissipate every few days. Future space missions will add to our understanding of small-scale processes, chemical composition, and vertical structure. Theoretical hypotheses about the interiors provide input for fluid dynamical models that reproduce many observed features of the winds, temperatures, and cloud patterns. In one set of models the winds are confined to the thin layer where clouds form. In other models, the winds extend deep into the planetary fluid interiors. Hypotheses will be tested further as observations and theories become more exact and detailed comparisons are made. 相似文献
8.
祁连山东部春季云参数特征与降水的关系研究 总被引：1，自引：1，他引：0
利用2005～2007年春季的降水和MODIS云资料,探讨了祁连山东部降雨（雪）与云量、云（冰）水路径、云层厚度等参数的关系。结果表明,降雪量与低云量、低云冰水路径、低云云顶-云底气压差呈明显的正相关,低云量多、低云冰水路径值大、气压差大,有利于降雪的产生;降雨量与低云云顶-云底气压差也呈明显的正相关,低云云层越厚,降雨量越大。通过卫星遥感获取的云参量与地面实测降水资料进行对应,可以为天气预报提供重要参考,还可为人工影响天气作业提供指导。 相似文献
9.
The ocean currents connecting the western tropical Pacific Ocean with the eastern tropical Pacific Ocean are driven by surface winds. The surface winds are in turn driven by the sea-surface temperature (SST) differences between these two regions. This dynamic coupling between the atmosphere and ocean may limit the SST in the tropical Pacific Ocean to below 305 kelvin even in the absence of cloud feedbacks. 相似文献
10.
依据苏州东桥试验区水稻生长期观测数据,采用多时相水稻拔节到抽穗期全极化Radarsat-2数据,分别分析了不同极化HH、VV、CROSS、比值HH/VV的雷达后向散射系数时域变化特征与生物量的相关关系,构建水云模型、二次多项式模型和指数模型反演水稻生物量。反演结果表明:HH、CROSS水云模型都有不错的反演效果,相关系数分别为0.910、0.902,而HH水云模型反演生物量尤佳,均方根误差为0.190。指数模型普遍优于二次多项式模型,HH/VV指数模型效果出众,相关系数为0.929,均方根误差为0.164。通过比较分析不同极化的水云模型、二次多项式模型和指数模型,HH水云模型与HH/VV指数模型反演水稻生物量精度相对较高。 相似文献
11.
The cloud-level atmosphere of Venus takes little more than 4 days to complete one rotation, whereas the solid planet below has a 243-day period. Computer simulations of the circulation of the Venus middle atmosphere between 40 and 85 kilometers, as driven by solar radiation absorbed in the clouds, reproduce (i) the observed cloud-level rotation rate, (ii) strong vertical shears above and below the cloud tops, and (iii) midlatitude jets and strong poleward flow on the day side. Simulated circulations converge to yield nearly the same zonal winds when initialized with both stronger or weaker rotation rates. These results support the hypothesis that the observed cloud-top rotation rate is maintained by statistical balance between fluxes of momentum by thermal tides and momentum advection by mean meridional circulation. 相似文献
12.
When the production of cloud condensation nuclei in the stratocumulus-topped marine boundary layer is low enough, droplet collisions can reduce concentrations of cloud droplet numbers to extremely low values. At low droplet concentrations a cloud layer can become so optically thin that cloud-top radiative cooling cannot drive vertical mixing. Under these conditions, model simulations indicate that the stratocumulus-topped marine boundary layer collapses to a shallow fog layer. Through this mechanism, marine stratiform clouds may limit their own lifetimes. 相似文献
13.
Crisp D Sinton WM Hodapp KW Ragent B Gerbault F Goebel JH Probst RG Allen DA Pierce K Stapelfeldt KR 《Science (New York, N.Y.)》1989,246(4929):506-509
Near-infrared images of the Venus night side show bright contrast features that move from east to west, in the direction of the cloud-top atmospheric superrotation. Recently acquired images of the Venus night side along with earlier spectroscopic observations allow identification of the mechanisms that produce these features, their level of formation, and the wind velocities at those levels. The features are detectable only at wavelengths near 1.74 and 2.3 micrometers, in narrow atmospheric windows between the CO(2) and H(2)O bands. The brightest features have brightness temperatures near 480 Kelvin, whereas the darkest features are more than 50 Kelvin cooler. Several factors suggest that this radiation is emitted by hot gases at altitudes below 35 kilometers in the Venus atmosphere. The feature contrasts are produced as this thermal radiation passes through a higher, cooler, atmospheric layer that has horizontal variations in transparency. The 6.5-day east-west rotation period of the features indicates that equatorial wind speeds are near 70 meters per second in this upper layer. Similar wind speeds have been measured by entry probes and balloons at altitudes between 50 and 55 kilometers in the middle cloud layer. The bright features indicate that there are partial clearings in this cloud deck. The presence of these clearings could decrease the efficiency of the atmospheric greenhouse that maintains the high surface temperatures on Venus. 相似文献
14.
以常规观测、卫星云图等资料对2016年1月22—24日聊城市寒潮天气过程的环流背景、物理量场等方面进行分析,得到此次寒潮天气过程的变化及对农业的影响。结果表明:大西洋暖脊在高纬东伸,促使乌拉尔山地区的弱脊不断发展形成阻高形势,是冷空气发展加强的有利条件;近地面冷高压势力强盛,受强冷平流影响,此次寒潮过程产生大风降温天气,气温持续降低,另外良好的水汽条件 都是产生降雪的原因;从卫星云图可以看到横槽槽线前陕西、山西和河北中部地区形成的一条宽广的层状云云带产生降雪天气,横槽转竖后云带后边缘光滑,也表示着强大的地面冷高压。 相似文献
15.
利用常规气象资料,对2010年3月19～20日山西省一次罕见大风天气的天气形势及主要影响要素进行了综合分析。结果表明：高空不稳定小槽和地面冷锋是引发这次罕见大风的主要天气系统。高空急流、风速垂直切变、气压梯度、3 h变压、冷暖平流、散度场等要素对大风的发生起到了一定的作用。在综合分析大风形成物理机制的基础上,得出了大风天气的预报着眼点,为大风预报提供理论依据,以期提高大风天气的预报准确率,减轻大风天气对社会及人类造成的危害。 相似文献
16.
Preliminary results of the nephelometer experiments conducted aboard the large sounder, day, north, and night probes of the Pioneer Venus mission are presented. The vertical structures of the Venus clouds observed simultaneously at each of the four locations from altitudes of from 63 kilometers to the surface are compared, and similarities and differences are noted. Tentative results from attempting to use the data from the nephelometer and cloud particle size spectrometer on the sounder probe to identify the indices of refraction of cloud particles in various regions of the Venus clouds are reported. Finally the nephelometer readings for the day probe during impact on the surface of Venus are presented. 相似文献
17.
Preston RA Hildebrand CE Purcell GH Ellis J Stelzried CT Finley SG Sagdeev RZ Linkin VM Kerzhanovich VV Altunin VI Kogan LR Kostenko VI Matveenko LI Pogrebenko SV Strukov IA Akim EL Alexandrov YN Armand NA Bakitko RN Vyshlov AS Bogomolov AF Gorchankov YN Selivanov AS Ivanov NM Tichonov VF Blamont JE Boloh L Laurans G Boischot A Biraud F Ortega-Molina A Rosolen C Petit G 《Science (New York, N.Y.)》1986,231(4744):1414-1416
A global array of 20 radio observatories was used to measure the three-dimensional position and velocity of the two meteorological balloons that were injected into the equatorial region of the Venus atmosphere near Venus midnight by the VEGA spacecraft on 11 and 15 June 1985. Initial analysis of only radial velocities indicates that each balloon was blown westward about 11,500 kilometers (8,000 kilometers on the night side) by zonal winds with a mean speed of about 70 meters per second. Excursions of the data from a model of constant zonal velocity were generally less than 3 meters per second; however, a much larger variation was evident near the end of the flight of the second balloon. Consistent systematic trends in the residuals for both balloons indicate the possibility of a solar-fixed atmospheric feature. Rapid variations in balloon velocity were often detected within a single transmission (330 seconds); however, they may represent not only atmospheric motions but also self-induced aerodynamic motions of the balloon. 相似文献
18.
Smith BA Soderblom LA Beebe R Bliss D Boyce JM Brahic A Briggs GA Brown RH Collins SA Cook AF Croft SK Cuzzi JN Danielson GE Davies ME Dowling TE Godfrey D Hansen CJ Harris C Hunt GE Ingersoll AP Johnson TV Krauss RJ Masursky H Morrison D Owen T Plescia JB Pollack JB Porco CC Rages K Sagan C Shoemaker EM Sromovsky LA Stoker C Strom RG Suomi VE Synnott SP Terrile RJ Thomas P Thompson WR Veverka J 《Science (New York, N.Y.)》1986,233(4759):43-64
Voyager 2 images of the southern hemisphere of Uranus indicate that submicrometersize haze particles and particles of a methane condensation cloud produce faint patterns in the atmosphere. The alignment of the cloud bands is similar to that of bands on Jupiter and Saturn, but the zonal winds are nearly opposite. At mid-latitudes (-70 degrees to -27 degrees ), where winds were measured, the atmosphere rotates faster than the magnetic field; however, the rotation rate of the atmosphere decreases toward the equator, so that the two probably corotate at about -20 degrees . Voyager images confirm the extremely low albedo of the ring particles. High phase angle images reveal on the order of 10(2) new ringlike features of very low optical depth and relatively high dust abundance interspersed within the main rings, as well as a broad, diffuse, low optical depth ring just inside the main rings system. Nine of the newly discovered small satellites (40 to 165 kilometers in diameter) orbit between the rings and Miranda; the tenth is within the ring system. Two of these small objects may gravitationally confine the e ring. Oberon and Umbriel have heavily cratered surfaces resembling the ancient cratered highlands of Earth's moon, although Umbriel is almost completely covered with uniform dark material, which perhaps indicates some ongoing process. Titania and Ariel show crater populations different from those on Oberon and Umbriel; these were probably generated by collisions with debris confined to their orbits. Titania and Ariel also show many extensional fault systems; Ariel shows strong evidence for the presence of extrusive material. About halfof Miranda's surface is relatively bland, old, cratered terrain. The remainder comprises three large regions of younger terrain, each rectangular to ovoid in plan, that display complex sets of parallel and intersecting scarps and ridges as well as numerous outcrops of bright and dark materials, perhaps suggesting some exotic composition. 相似文献
19.
Data from the Pioneer Venus cloud particle size spectrometer experiment has revealed the Venus cloud system to be a complicated mixture of particles of various chemical composition distinguishable by their multimodal size distributions. The appearance, disappearance, growth, and decay of certain size modes has aided the preliminary identification of both sulfuric acid and free sulfur cloud regions. The discovery of large particles > 30 micrometers, significant particle mass loading, and size spectral features suggest that precipitation is likely produced; a peculiar aerosol structure beneath the lowest cloud layer could be residue from a recent shower. 相似文献
20.
【目的】研究温室葡萄不同受光架式和冠位叶片组织结构及其叶绿体超微结构的变化,为温室葡萄栽培提供理论依据。【方法】以温室的棚架、单篱架、双篱架葡萄为试材,分别采用光学显微和电子显微镜技术观测不同架式和冠位叶片的显微结构和叶绿体的超微结构。【结果】温室葡萄棚架受光优于篱架,篱架下部叶片受光极差,阴天对篱架受光的影响比棚架大,对下部影响比上部大;温室葡萄叶片的总厚、栅栏组织厚、组织密度CTR值及栅栏海绵组织比值等光合组织结构有所退化,但不同受光架式间和冠位间有差异。棚架的叶片质量均匀,光合组织发达,篱架的下部叶片结构严重退化;叶片总厚、栅栏组织厚与光照强度呈显著正相关;葡萄棚架叶片和篱架上部叶片的叶绿体数、基粒数、基粒片层数明显高于篱架下部的叶片。【结论】温室葡萄采取棚架栽培时整体叶片的叶绿体发育正常,而篱架下部叶片因长期弱光胁迫导致叶绿体结构发生异常变化。 相似文献