雷电滤波器     

金能均 《东北地震研究》1992,(2)

本文叙述了两种雷电滤波器的工作原理及其使用方法。  相似文献   

GPS-derived horizontal ice flow velocities along the traverse route from Zhongshan Station to Dome-A, East Antarctica     

王清华 《极地研究(英文版)》2003,14(1)

1　IntroductionFromitsoriginalformulationin 1 990 ,theInternationalTrans AntarcticScientificExpedition (ITASE)hashadasitsprimaryaimthecollectionandinterpretationofacon tinental widearrayofenvironmentalparametersassembledthroughthecoordinatedeffortsofscientistsfromseveralnations(Mayewskietal.1 996) .AsaconsequenceITASEhasbeenfocusedtoaddresstwokeyscientificobjectives:1 )Todeterminethespatialvariabil ityofAntarcticclimate (eg.accumulation,airtemperature,atmosphericcirculation)overthelast2…  相似文献   

MULTI-DIMENSIONAL NUMERICAL STUDIES OF CONVECTION-RELATED STELLAR PROBLEMS     

Chan Kwing Lam 《紫金山天文台台刊》2003,(2)

1　IntroductionManybottlenecksinthetheoreticalstudyofstellarevolutionarisefromthelackofunder standingofsomehighlycomplicatedprocessesthatcannotbetreatedwithanalyticaltech niques .Alargeportionoftheseprocessesisrelatedtohydrodynamics,particularlyconvec tion .Theapplicationofmultidimensionalnumericalcomputationstotheinvestigationofthesedifficultproblemshasmadegreatprogressinrecentyears .Here ,weprovideasurveyoftherecentnumericalstudiesofconvectionrelatedproblems.Theobjectiveistoassistthosewhoar…  相似文献   

几个天然镁铝榴石的穆斯堡尔效应的研究          下载免费PDF全文

中国科学院地质研究所矿物物理组计算组  中国科学院高能物理研究所核技术应用组 《地质科学》1977,12(1):93-103

穆斯堡尔效应是一种无反冲的核γ射线的共振吸收现象,它是1958年由穆斯堡尔(R.L.M(?)ssbauer)发现的。由于穆斯堡尔效应产生的γ射线共振吸收谱线的能量宽度接近原子核能级的自然线宽,以及无反冲γ射线共振吸收(或散射)对γ射线能量变化十分灵敏,因此,可以把共振吸收的原子核当做灵敏的探针,测量固体中有关的原子核与核所在位置上固体的化学环境间的超精细相互作用。近些年来,穆斯堡尔效应已广泛应用于物理学、化学、生物学及矿物学的研究中来,穆斯堡尔谱仪已成为这些学科的重要研究工具之一。  相似文献   

Analysis and interpretation of Cassini Titan radar altimeter echoes     

Howard A. Zebker  Yonggyu Gim  Scott Hensley  Cassini Radar Team 《Icarus》2009,200(1):240-255

The Cassini spacecraft has acquired 25 radar altimeter elevation profiles along Titan's surface as of April 2008, and we have analyzed 18 of these for which there are currently reconstructed ephemeris data. Altimeter measurements were collected at spatial footprint sizes from 6-60 km along ground tracks of length 400-3600 km. The elevation profiles yield topographic information at this resolution with a statistical height accuracy of 35-50 m and kilometer-scale errors several times greater. The data exhibit significant variations in terrain, from flat regions with little topographic expression to very rugged Titanscapes. The bandwidth of the transmitted waveform admits vertical resolution of the terrain height to 35 m at each observed location on the surface. Variations in antenna pointing and changes in surface statistics cause the range-compressed radar echoes to exhibit strong systematic and time-variable biases of hundreds of meters in delay. It is necessary to correct the received echoes for these changes, and we have derived correction algorithms such that the derived echo profiles are accurate at the 100 m level for off-nadir pointing errors of 0.3° and 0.6°, for leading edge and echo centroid estimators, respectively. The leading edge of the echo yields the elevation of the highest points on the surface, which we take to be the peaks of any terrain variation. The mean value of the echo delay is more representative of the mean elevation, so that the difference of these values gives an estimate of any local mountain heights. Finding locations where these values diverge indicates higher-relief terrain. Elevation features are readily seen in the height profiles. Several of the passes show mountains of several hundred m altitude, spread over 10's or even 100's of km in spatial extent, so that slopes are very small. Large expanses of sub-100 m topography are commonplace on Titan, so it is rather smooth in many locations. Other areas exhibit more relief, although the overall observed variation in surface height on any pass is less than about 1 km. Some elevation features correspond to observed changes in brightness in Cassini infrared images, but many do not. Correspondence between the imaging SAR ground tracks and the altimeter paths is limited, so that identifying elevation changes with higher resolution SAR features is premature at present.  相似文献   

Titan's surface at 2.2-cm wavelength imaged by the Cassini RADAR radiometer: Calibration and first results     

M.A. Janssen  R.D. Lorenz  F. Paganelli  R.L. Kirk  S.D. Wall  Y. Anderson  P. Callahan  G.A. Hamilton  L. Roth  A. Le Gall  the Cassini Radar Team 《Icarus》2009,200(1):222-239

The first comprehensive calibration and mapping of the thermal microwave emission from Titan's surface is reported based on radiometric data obtained at 2.2-cm wavelength by the passive radiometer included in the Cassini Radar instrument. The data reported were accumulated from 69 separate observational segments in Titan passes from Ta (October 2004) through T30 (May 2007) and include emission from 94% of Titan's surface. They are diverse in the key observing parameters of emission angle, polarization, and spatial resolution, and their reduction into calibrated global mosaic maps involved several steps. Analysis of the polarimetry obtained at low to moderate resolution (50+ km) enabled integration of the radiometry into a single mosaic of the equivalent brightness temperature at normal incidence with a relative precision of about 1 K. The Huygens probe measurement of Titan's surface temperature and radiometry obtained on Titan's dune fields allowed us to infer an absolute calibration estimated to be accurate to a level approaching 1 K. The results provide evidence for a surface that is complex and varied on large scales. The radiometry primarily constrains physical properties of the surface, where we see strong evidence for subsurface (volume) scattering as a dominant mechanism that determines the emissivity, with the possibility of a fluffy or graded-density surface layer in many regions. The results are consistent with, but not necessarily definitive of a surface composition resulting from the slow deposition and processing of organic compounds from the atmosphere.  相似文献   

Fundamentally distinct outcomes of asteroid collisional evolution and catastrophic disruption     

Andrew F. Cheng  The Hayabusa Team 《Planetary and Space Science》2009,57(2):165-172

The outcomes of asteroid collisional evolution are presently unclear: are most asteroids larger than 1 km size gravitational aggregates reaccreted from fragments of a parent body that was collisionally disrupted, while much smaller asteroids are collisional shards that were never completely disrupted? The 16 km mean diameter S-type asteroid 433 Eros, visited by the NEAR mission, has surface geology consistent with being a fractured shard. A ubiquitous fabric of linear structural features is found on the surface of Eros and probably indicates a globally consolidated structure beneath its regolith cover. Despite the differences in absolute scale and in lighting conditions for NEAR and Hayabusa, similar features should have been found on 25143 Itokawa if present. This much smaller, 320 m diameter S-asteroid was visited by the Hayabusa spacecraft. Comparative analyses of Itokawa and Eros geology reveal fundamental differences, and interpretation of Eros geology is illuminated by comparison with Itokawa. Itokawa lacks a global lineament fabric, and its blocks, craters, and regolith may be inconsistent with formation and evolution as a fractured shard, unlike Eros. An object as small as Itokawa can form as a rubble pile, while much larger Eros formed as a fractured shard. Itokawa is not a scaled-down Eros, but formed by catastrophic disruption and reaccumulation.  相似文献   

Dunes on Titan observed by Cassini Radar     

J. Radebaugh  R.D. Lorenz  S.D. Wall  E. Reffet  R.M. Lopes  L. Soderblom  M. Janssen  P. Callahan  the Cassini Radar Team 《Icarus》2008,194(2):690-703

Thousands of longitudinal dunes have recently been discovered by the Titan Radar Mapper on the surface of Titan. These are found mainly within ±30° of the equator in optically-, near-infrared-, and radar-dark regions, indicating a strong proportion of organics, and cover well over 5% of Titan's surface. Their longitudinal duneform, interactions with topography, and correlation with other aeolian forms indicate a single, dominant wind direction aligned with the dune axis plus lesser, off-axis or seasonally alternating winds. Global compilations of dune orientations reveal the mean wind direction is dominantly eastwards, with regional and local variations where winds are diverted around topographically high features, such as mountain blocks or broad landforms. Global winds may carry sediments from high latitude regions to equatorial regions, where relatively drier conditions prevail, and the particles are reworked into dunes, perhaps on timescales of thousands to tens of thousands of years. On Titan, adequate sediment supply, sufficient wind, and the absence of sediment carriage and trapping by fluids are the dominant factors in the presence of dunes.  相似文献   

V. A. Ambartsumian— a life in science     

The editorial board of the journal Astrofizika 《Astrophysics》2008,51(3):280-293

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第十五批天文学名词的推荐译名     

中国天文学会天文学名词审定委员会 《天文学进展》2008,26(1):95-99

中国天文学会名词审定委员会从1985年开始在<天文学进展>发表天文学名词的推荐译名,到2007年已公布了14批2280个名词.现再推荐第十五批151个名词,其中大多数是近年来出现的天文学新词.希望读者在试用过程中对译名提出改进意见.  相似文献