共查询到20条相似文献，搜索用时 31 毫秒
1.
A random-code technique has been used at Arecibo to obtain delay-Doppler radar images of the full disk of Mercury. Anomalously bright features were found at the north and south poles. The north polar feature is oblong (4 degrees by 8 degrees ) and offset from the pole. The smaller south polar feature is mostly confined to the floor of the crater Chao Meng-Fu. The polar locations and radar properties of these features indicate that they may be produced by volume scattering in ice. The images also reveal a variety of more subdued reflectivity features ranging in size from hundreds to thousands of kilometers; some of these appear to have an impact origin. 相似文献
2.
Recent radar observations of Mercury have revealed the presence of anomalous radar reflectivity and polarization features near its north and south poles. Thermal model calculations show that, despite Mercury's proximity to the sun, the temperatures of flat, low-reflectivity surfaces at Mercury's poles are not expected to exceed 167 kelvin. The locations of the anomalous polar radar features appear to be correlated with the locations of large, high-latitude impact craters. Maximum surface temperatures in the permanently shadowed regions of these craters are expected to be significantly colder, as low as 60 kelvin in the largest craters. These results are consistent with the presence of water ice, because at temperatures lower than 112 kelvin, water ice should be stable to evaporation over time scales of billions of years. 相似文献
3.
Full disk images of Mars have been obtained with the use of the Very Large Array (VLA) to map the radar reflected flux density. The transmitter system was the 70-m antenna of the Deep Space Network at Goldstone, California. The surface of Mars was illuminated with continuous wave radiation at a wavelength of 3,5 cm. The reflected energy was mapped in individual 12-minute snapshots with the VLA in its largest configuration; fringe spacings as small as 67 km were obtained. The images reveal near-surface features including a region in the Tharsis volcano area, over 2000 km in east-west extent, that displayed no echo to the very low level of the radar system noise. The feature, called Stealth, is interpreted as a deposit of dust or ash with a density less than about 0.5 gram per cubic centimeter and free of rocks larger than 1 cm across. The deposit must be several meters thick and may be much deeper. The strongest reflecting geological feature was the south polar ice cap, which was reduced in size to the residual south polar ice cap at the season of observation. The cap image is interpreted as arising from nearly pure CO(2) or H(2)O ice with a small amount of martian dust (less than 2 percent by volume) and a depth greater than 2 to 5 m. Only one anomalous reflecting feature was identified outside of the Tharsis region, although the Elysium region was poorly sampled in this experiment and the north pole was not visible from Earth. 相似文献
4.
Herkenhoff KE Byrne S Russell PS Fishbaugh KE McEwen AS 《Science (New York, N.Y.)》2007,317(5845):1711-1715
Mars' north pole is covered by a dome of layered ice deposits. Detailed ( approximately 30 centimeters per pixel) images of this region were obtained with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter (MRO). Planum Boreum basal unit scarps reveal cross-bedding and show evidence for recent mass wasting, flow, and debris accumulation. The north polar layers themselves are as thin as 10 centimeters but appear to be covered by a dusty veneer in places, which may obscure thinner layers. Repetition of particular layer types implies that quasi-periodic climate changes influenced the stratigraphic sequence in the polar layered deposits, informing models for recent climate variations on Mars. 相似文献
5.
Cutts JA Blasius KR Briggs GA Carr MH Greeley R Masursky H 《Science (New York, N.Y.)》1976,194(4271):1329-1337
During October 1976, the Viking 2 orbiter acquired approximately 700 high-resolution images of the north polar region of Mars. These images confirm the existence at the north pole of extensive layered deposits largely covered over with deposits of perennial ice. An unconformity within the layered deposits suggests a complex history of climate change during their time of deposition. A pole-girdling accumulation of dunes composed of very dark materials is revealed for the first time by the Viking cameras. The entire region is devoid of fresh impact craters. Rapid rates of erosion or deposition are implied. A scenario for polar geological evolution, involving two types of climate change, is proposed. 相似文献
6.
Howard HT Tyler GL Esposito PB Anderson JD Reasenberg RD Shapiro II Fjeldbo G Kliore AJ Levy GS Brunn DL Dickinson R Edelson RE Martin WL Postal RB Seidel B Sesplaukis TT Shirley DL Stelzried CT Sweetnam DN Wood GE Zygielbaum AI 《Science (New York, N.Y.)》1974,185(4146):179-180
Analysis of the radio-tracking data from Mariner 10 yields 6,023,600 +/- 600 for the ratio of the mass of the sun to that of Mercury, in very good agreement with values determined earlier from radar data alone. Occultation measurements yielded values for the radius of Mercury of 2440 +/- 2 and 2438 +/- 2 kilometers at laditudes of 2 degrees N and 68 degrees N, respectively, again in close agreement with the average equatorial radius of 2439 +/- 1 kilometers determined from radar data. The mean density of 5.44 grams per cubic centimeter deduced for Mercury from Mariner 10 data thus virtually coincides with the prior determination. No evidence of either an ionosphere or an atmosphere was found, with the data yielding upper bounds on the electron density of about 1500 and 4000 electrons per cubic centimeter on the dayside and nightside, respectively, and an inferred upper bound on the surface pressure of 10(-8) millibar. 相似文献
7.
Luz D Berry DL Piccioni G Drossart P Politi R Wilson CF Erard S Nuccilli F 《Science (New York, N.Y.)》2011,332(6029):577-580
Initial images of Venus's south pole by the Venus Express mission have shown the presence of a bright, highly variable vortex, similar to that at the planet's north pole. Using high-resolution infrared measurements of polar winds from the Venus Express Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument, we show the vortex to have a constantly varying internal structure, with a center of rotation displaced from the geographic south pole by ~3 degrees of latitude and that drifts around the pole with a period of 5 to 10 Earth days. This is indicative of a nonsymmetric and varying precession of the polar atmospheric circulation with respect to the planetary axis. 相似文献
8.
The Infrared Thermal Mappers aboard the two Viking orbiters obtained solar reflectance and infrared emission measurements of the Martian north and south polar regions during an entire Mars year. The observations were used to determine annual radiation budgets, infer annual carbon dioxide frost budgets, and constrain spring season surface and atmospheric properties with the aid of a polar radiative model. The results provide further confirmation of the presence of permanent CO(2)frost deposits near the south pole and show that the stability of these deposits can be explained by their high reflectivities. In the north, the observed absence of solid CO(2) during summer was primarily the result of enhanced CO(2) sublimation rates due to lower frost reflectivities during spring. The results suggest that the present asymmetric behavior of CO(2)frost at the Martian poles is caused by preferential contamination of the north seasonal polar cap by atmospheric dust. 相似文献
9.
利用1961—2015年历史气象资料,普查石河子地区持续10 d以上≥35℃的高温过程,分析了石河子地区持续异常高温过程的环流形势以及太阳黑子年际变化与高温过程的对应关系;在此基础上分析了2015年7月中下旬的持续异常高温过程发生的物理机制,并对数值预报进行了检验。结果表明,石河子地区持续高温过程主要是在高压脊型和纬向带状型2种环流背景下发生,500 hPa 580 dagpm等高线北上越过天山进入北疆地区,极锋锋区北缩至60°N以北;850 hPa温度场上24℃等温线北上控制北疆地区;该地区高温过程多发生在太阳黑子活动低谷期;高温期间极涡在65°N以北至极地附近,位置显著偏西偏北;副热带高压显著发展,异常强大的暖高压、持续的下沉增温和地形效应造成了此次持续的高温过程;ECMWF模式准确预报了此次高温过程的环流形势和物理场,单站检验结果显示地面气压和850 hPa温度预报误差分别在2 hPa以内和1℃以内,环流形势场和要素预报稳定且时效长,检验结果表明ECMWF产品可以作为石河子地区连续高温过程预报的参考。 相似文献
10.
The images of the nucleus of comet Halley returned by the Giotto spacecraft reveal a number of active regions on the surface, one of which is near the expected location of the rotation pole. This feature is larger and brighter than other source regions, suggesting that the mechanism that drives this source is also different. At this active region near the rotation pole, the sun was circumpolar for a significant portion of the solar encounter. Continuous insolation heated the nucleus to greater depths than in other areas, producing the broad, active polar region. 相似文献
11.
Kieffer HH Chase SC Martin TZ Miner ED Palluconi FD 《Science (New York, N.Y.)》1976,194(4271):1341-1344
Broadband thermal and reflectance observations of the martian north polar region in late summer yield temperatures for the residual polar cap near 205 K with albedos near 43 percent. The residual cap and several outlying smaller deposits are water ice with included dirt; there is no evidence for any permanent carbon dioxide polar cap. 相似文献
12.
Spahn F Schmidt J Albers N Hörning M Makuch M Seiss M Kempf S Srama R Dikarev V Helfert S Moragas-Klostermeyer G Krivov AV Sremcevic M Tuzzolino AJ Economou T Grün E 《Science (New York, N.Y.)》2006,311(5766):1416-1418
During Cassini's close flyby of Enceladus on 14 July 2005, the High Rate Detector of the Cosmic Dust Analyzer registered micron-sized dust particles enveloping this satellite. The dust impact rate peaked about 1 minute before the closest approach of the spacecraft to the moon. This asymmetric signature is consistent with a locally enhanced dust production in the south polar region of Enceladus. Other Cassini experiments revealed evidence for geophysical activities near Enceladus' south pole: a high surface temperature and a release of water gas. Production or release of dust particles related to these processes may provide the dominant source of Saturn's E ring. 相似文献
13.
Zurbuchen TH Raines JM Slavin JA Gershman DJ Gilbert JA Gloeckler G Anderson BJ Baker DN Korth H Krimigis SM Sarantos M Schriver D McNutt RL Solomon SC 《Science (New York, N.Y.)》2011,333(6051):1862-1865
Global measurements by MESSENGER of the fluxes of heavy ions at Mercury, particularly sodium (Na(+)) and oxygen (O(+)), exhibit distinct maxima in the northern magnetic-cusp region, indicating that polar regions are important sources of Mercury's ionized exosphere, presumably through solar-wind sputtering near the poles. The observed fluxes of helium (He(+)) are more evenly distributed, indicating a more uniform source such as that expected from evaporation from a helium-saturated surface. In some regions near Mercury, especially the nightside equatorial region, the Na(+) pressure can be a substantial fraction of the proton pressure. 相似文献
14.
根据寒潮标准,对新疆东部哈密区域50年的寒潮天气进行统计。结果表明：新疆哈密地区寒潮最早出现在9月2～3日,最晚出现在5月22～23日;四季中春季出现最多,为101次,秋季41次,冬季27次;50年来哈密地区寒潮天气过程出现次数总体呈现减少趋势;哈密地区北部寒潮出现频次、强度高于哈密地区南部,初寒潮北部早于南部,终寒湖北部晚于南部;寒潮入侵路径主要有4条：西方路径、西北路径、北方路径和超极地路径。 相似文献
15.
[目的]研究桂林地区冰雹天气及其预报方法。[方法]针对桂林地区的冰雹发生情况,结合桂林新一代多普勒天气雷达的观测资料,总结分析影响桂林地区冰雹的天气形势和雷达回波特征,探索冰雹天气的短时临近预报方法。[结果]桂林地区每年都会出现1～2次冰雹,冰雹发生受地形影响明显,地理分布极不均匀;时间分布比较集中,主要发生在春季,且多发生在下午到傍晚时分。新一代多普勒天气雷达探测冰雹十分有效,桂林地区冰雹的回波单体强度≥50 dBz,回波顶高≥10 km,垂直液态水含量≥40 kg/m2,常配合有中气旋,冰雹很强的时候,还会出现三体散射特征。冰雹的预报以短时临近预报为主。[结论]该研究为冰雹的预报、人工消雹和减灾防灾工作提供参考。 相似文献
16.
The residual frost caps of Mars are probably water-ice. They may be the source of the water vapor associated with seasonal polar hoods. A permanent reservoir of solid CO(2) is also probably present within the north residual cap and may comprise a mass of CO(2) some two to five times that of the present atmosphere of Mars. The martian atmospheric pressure is probably regulated by the temperature of the reservoir and not by the annual heat balance of exposed solid CO(2) (37). The present reservoir temperature presumably reflects a long-term average of the polar heat balance. The question of a large permanent north polar cap is reexamined in light of the Mariner 9 data. The lower general elevation of the north polar region compared to the south and the resulting occurrence in the north of a permanent CO(2) deposit are probably responsible for the differences in size and shape of the two residual caps. The details of the processes involved are less apparent, however. It might be argued that the stability of water-ice deposits depends on both insolation and altitude. The present north and south residual caps should be symmetrically located with respect to such a hypothetical stability field. However, the offset of the south cap from the geometrical pole, the non-symmetrical outline of the north cap, and the apparently uniform thickness of the thin, widespread water-ice all argue against control by simple solid-vapor equilibrium of water under present environmental conditions. We think that the present location of the water-ice may reflect, in part, the past location of the permanent CO(2) reservoir. The extreme stability of polar water-ice deposits increases the likelihood that past environmental conditions may be recorded there. Detailed information on elevations in the vicinity of the residual caps is needed before we can further elucidate the nature and history of the residual caps. This, along with measurements of polar infrared emission, should be given high priority in future missions to Mars. Two conclusions follow from the limitation of the mass of solid CO(2) on Mars at present to two to five times the mass of CO(2) in the atmosphere. If all of this CO(2) was entirely sublimated into the atmosphere as a result of hypothetical astronomical or geophysical effects, the average surface pressure would increase to 15 to 30 mbar. Although such a change would have considerable significance for eolian erosion and transportation, there seems to be little possibility that a sufficiently earthlike atmosphere could result for liquid water to become an active erosional agent, as postulated by Milton (38). The pressure broadening required for a green-house effect requires at least 10 to 20 times more pressure (39). If liquid water was ever active in modifying the martian surface, it must have been at an earlier epoch, before the present, very stable CO(2)/H(2)O system developed. There can be no intermittent earthlike episodes now. Furthermore, the present abundance of CO(2) on Mars may be an indicator of the cumulative evolution of volatiles to the surface of the planet (40). Thus, even the possibility of an earlier earth-like episode is dimmed. On Mars, the total CO(2) definitely outgassed has evidently been about 60 +/- 20 g/cm(2). On the earth, about 70 +/- 30 kg/cm(2) of CO(2) have been released to the surface (41). Hence, the total CO(2) devolved by Mars per unit area is about 0.1 percent of that evolved by the earth. Thus, the observational limits we place on solid CO(2) presently located under the north residual cap also may constitute considerable constraints on the total differentiation and devolatilization of the planet. If they are valid, it would seem unlikely that Mars has devolatilized at all like the earth, or ever experienced an earthlike environment on its surface. 相似文献
17.
Ground-based observations of two conspicuous features near the north pole of Saturn, the polar vortex and the hexagonal wave structure, were made from July 1990 to October 1991, 10 years after their discovery. During this period the polar spot drifted in longitude, relative to system III, by -0.0353 degrees per day on average. Superimposed on this mean motion, the spot also underwent short-term rapid excursions in longitude of up to approximately 14 degrees at rates of up to approximately 1 degrees per day. The spot also exhibited irregular variations in its latitude location. A combination of these data together with those obtained by Voyager 1 and 2 in 1980 and 1981 shows that the spot drifted -0.0577 degrees per day for the 11-year interval from 1980 to 1991. The large lifetime of both features indicates that they are insensitive to the strong variations in the seasonal heating of the cloud layers in the upper polar atmosphere. 相似文献
18.
Porco CC West RA McEwen A Del Genio AD Ingersoll AP Thomas P Squyres S Dones L Murray CD Johnson TV Burns JA Brahic A Neukum G Veverka J Barbara JM Denk T Evans M Ferrier JJ Geissler P Helfenstein P Roatsch T Throop H Tiscareno M Vasavada AR 《Science (New York, N.Y.)》2003,299(5612):1541-1547
The Cassini Imaging Science Subsystem acquired about 26,000 images of the Jupiter system as the spacecraft encountered the giant planet en route to Saturn. We report findings on Jupiter's zonal winds, convective storms, low-latitude upper troposphere, polar stratosphere, and northern aurora. We also describe previously unseen emissions arising from Io and Europa in eclipse, a giant volcanic plume over Io's north pole, disk-resolved images of the satellite Himalia, circumstantial evidence for a causal relation between the satellites Metis and Adrastea and the main jovian ring, and information on the nature of the ring particles. 相似文献
19.
Ho GC Krimigis SM Gold RE Baker DN Slavin JA Anderson BJ Korth H Starr RD Lawrence DJ McNutt RL Solomon SC 《Science (New York, N.Y.)》2011,333(6051):1865-1868
The MESSENGER spacecraft began detecting energetic electrons with energies greater than 30 kilo-electron volts (keV) shortly after its insertion into orbit about Mercury. In contrast, no energetic protons were observed. The energetic electrons arrive as bursts lasting from seconds to hours and are most intense close to the planet, distributed in latitude from the equator to the north pole, and present at most local times. Energies can exceed 200 keV but often exhibit cutoffs near 100 keV. Angular distributions of the electrons about the magnetic field suggest that they do not execute complete drift paths around the planet. This set of characteristics demonstrates that Mercury's weak magnetic field does not support Van Allen-type radiation belts, unlike all other planets in the solar system with internal magnetic fields. 相似文献
20.
Alexandrov YN Crymov AA Kotelnikov VA Petrov GM Rzhiga ON Sidorenko AI Sinilo VP Zakharov AI Akim EL Basilevski AT Kadnichanski SA Tjuflin YS 《Science (New York, N.Y.)》1986,231(4743):1271-1273
From October 1983 to July 1984, the north hemisphere of Venus, from latitude 30 degrees to latitude 90 degrees , was mapped by means of the radar imagers and altimeters of the spacecraft Venera 15 and Venera 16. This report presents the results of the radar mapping of the Maxwell Montes region, one of the most interesting features of Venus' surface. A radar mosaic map and contour map have been compiled. 相似文献