基于变形信息分解的大坝变形趋势判断及预测研究     

郝永河  郝永艳  唐承忠  杨华 《大地测量与地球动力学》2021,41(8):841-845

在分离大坝变形数据信息的基础上,利用重标极差法实现大坝变形趋势判断,然后利用优化极限学习机及混沌理论实现大坝变形预测。重标极差分析表明,大坝变形始终具有正向持续性,但其程度具有减弱趋势。在变形预测过程中,模型参数的递进优化不仅能提高预测精度,还能有效提高其稳定性,预测模型的相对误差均值均小于2%,验证了本文预测思路的有效性。大坝变形趋势判断及预测结果一致性较好,均认为大坝变形仍会进一步增加,但增加幅度相对较小,趋向于稳定发展。  相似文献   

基于光学遥感影像的2019年加利福尼亚M_W7.1和M_W6.4双震同震形变测量     

傅志豪  王鑫  张景发 《大地测量与地球动力学》2021,41(5):506-510

利用地震前后的Landsat-8和Sentinel-2光学遥感影像数据,基于频率域互相关算法提取加利福尼亚州MW7.1及MW6.4地震的同震形变场,同时针对形变数据易受轨道误差、条带误差及时间失相干的影响,分别采用最小二乘多项式曲线拟合、改进均值相减等方法去除系统误差项。研究表明,MW7.1主震以右旋走滑为主,地表形变的断层迹线呈NNW走向,长度达55 km,最大滑移量约为2.82 m;MW6.4地震的发震断层迹线呈NE走向,长度达15 km,最大滑移量约为1.05 m,推测2次地震的发震断层分别为NNW向右旋走滑断裂及NE向左旋走滑断裂,二者形成典型的共轭关系。  相似文献   

顾及三维方向的GNSS坐标时间序列粗差探测方法     

许炜  吕志平  董行  邝英才  杨凯淳  黄辉 《大地测量与地球动力学》2021,41(10):1018-1023

针对GNSS坐标时间序列中粗差为三维位置粗差的特点,提出综合三维坐标的迭代最小二乘粗差探测方法。通过实验模拟数据,分别利用3倍中误差（3σ）准则和四分位距（interquartile range, IQR）准则对单方向和综合N、E、U三方向的粗差进行探测。结果表明,2种判别准则中,综合考虑3个方向的探测效果远好于单方向的探测效果,且探测效率均超过95%;3σ准则的探测效率稍高于IQR准则,但误判率也较高。在实测数据中的应用表明,SOPAC(Scrips Orbit and Permanent Array Center)提供的部分raw类型全球IGS站时间序列中粗差占0.1%~4.7%;运用IQR准则综合3个方向的粗差探测得到的时间序列要比cleaned trend类型更加干净。  相似文献   

秦岭凤太铅锌-金矿集区成矿规律与找矿预测     

王瑞廷  张革利  李青锋  张斌  成欢  冀月飞 《地球科学与环境学报》2021,(3):528-548

凤太铅锌-金矿集区地处秦岭泥盆系贵金属-多金属成矿带西段,总体为夹持于湘子河断裂、酒奠梁断裂之间,以NWW向褶皱和NWW向断裂组合而成的近似菱形构造块体,主要出露的泥盆系为浅变质碳酸盐岩与细碎屑岩建造,东部出露的花红树坪岩体、西坝岩体和集中分布的岩脉为区内铅锌、金成矿提供了物质及热动力。典型矿床解剖结果表明:铅锌矿床受控于区域断裂及背斜构造且产出于特定的岩性层,与铅锌成矿关系密切的物理化学条件转换界面是中泥盆统古道岭组与上泥盆统星红铺组之间接触界面(硅钙面),铅锌矿床多位于面状高磁异常与低磁异常过渡部位并显示Pb-Zn-Hg-Cd组合化探异常,表明铅锌矿床成因类型为层控岩浆热液型;已知含矿背斜走向与倾向延伸部位、与其有相似成矿条件的次级背斜、大面积千枚岩覆盖区深部隐伏背斜的鞍部及倾斜部位是铅锌找矿有利地段。金矿床受控于断裂构造带或其旁侧的脆-韧性剪切带及其叠加部位,多位于高磁异常带中局部高磁异常向低磁异常过渡部位,与Au-Ag-(As-W-Bi-Sb)组合化探异常吻合度高,岩浆活动与金成矿关系密切,表明金矿床为中低温岩浆热液型;已探明大型金矿床近外围及深部是金找矿重点靶区。铅锌、金矿床均属于印支期与碰撞造山岩浆期后热液有关的铅锌、铜、金矿床成矿系列。基于成矿地质体、成矿构造、成矿结构面与矿体的相互作用与位置关系,建立了凤太铅锌-金矿集区铅锌、金成矿模式;叠加典型矿床物化探、遥感异常特征,构建找矿预测综合信息模型;采用“证据权法”,预测找矿靶区6处,说明区内找矿潜力大,下一步找矿工作重点是对隐伏控矿构造与隐伏矿体的预测与探索。  相似文献   

Hα emission objects in Circinus     

S. Noroozi  M. Haas  Z. Chen  R. Chini 《Astronomische Nachrichten》2013,334(3):282-287

We present a new survey for Hα emission objects in the Circinus cloud complex and introduce an efficient photometric method for detecting Hα emission via observations in a narrow‐band filter. The observed flux is compared to a blackbody fit of the continuum. Our search strategy reveals 20 stars with strong Hα emission (EW > 10 Å), eight of them being new detections. All Hα stars display infrared excess corroborating their youth. On the other hand, the region contains a number of infrared excess objects that do not show Hα emission. Our results support the picture that accretion – as witnessed by Hα emission – is a highly variable phenomenon. Therefore, Hα surveys can only trace the temporarily active objects. In contrast, infrared excess is a more robust tracer that reveals most of the population of young stellar objects in a star forming region. Our analysis of the general stellar content of the region yields a reliable distance of 450 pc for the Circinus cloud. Moreover, we find a ratio of total‐to‐selective extinction of R^V = 2.8 suggesting that smaller‐than‐normal dust grains may be present. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Long‐term photometry of three active red giants in close binary systems: V2253 Oph,IT Com and IS Vir     

K. Olh  A. Mor  K.G. Strassmeier  T. Borkovits  T. Granzer 《Astronomische Nachrichten》2013,334(7):625-637

We present and analyze long‐term optical photometric measurements of the three active stars V2253 Oph, IT Com and IS Vir. All three systems are single‐lined spectroscopic binaries with an early K giant as primary component but in different stages of orbital‐rotational synchronization. Our photometry is supplemented by 2MASS and WISE near‐IR and mid‐IR magnitudes and then used to obtain more accurate effective temperatures and extinctions. For V2253 Oph and IT Com, we found their spectral energy distributions consistent with pure photospheric emission. For IS Vir, we detect a marginal mid‐IR excess which hints towards a dust disk. The orbital and rotational planes of IT Com appear tobe coplanar, contrary to previous findings in the literature. We apply a multiple frequency analysis technique to determine photometric periods, and possibly changes of periods, ranging from days to decades. New rotational periods of 21.55±0.03 d, 65.1±0.3 d, and 23.50±0.04 d were determined for V2253 Oph, IT Com, and IS Vir, respectively. Splitting of these periods led to tentative detections of differential surface rotations of δP/P ≈ 0.02 for V2253 Oph and 0.07 for IT Com. Using a time‐frequency technique based on short‐term Fourier transforms we present evidence of cyclic light variations of length ≈ 10 yr for V2253 Oph and 5–6 yr for IS Vir. A single flip‐flop event has been observed for IT Com of duration 2–3 yr. Its exchange of the dominant active longitude had happened close to a time of periastron passage, suggesting some response of the magnetic activity from the orbital dynamics. The 21.55‐d rotational modulation of V2253 Oph showed phase coherence also with the orbital period, which is 15 times longer than the rotational period, thus also indicating a tidal feedback with the stellar magnetic activity. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

The density and temperature structure near the exobase of Saturn from Cassini UVIS solar occultations     

T.T. Koskinen  B.R. Sandel  R.V. Yelle  F.J. Capalbo  G.M. Holsclaw  W.E. McClintock  S. Edgington 《Icarus》2013

We analyzed 15 solar occultations observed by the Cassini UVIS instrument to constrain the density and temperature structure near the exobase of Saturn. We retrieved the density of H₂ and thus the temperature at altitudes higher than 1900 km above the 1 bar level by analyzing the ionization continuum of H₂ at wavelengths shorter than 804 Å. We find that the exospheric temperature ranges from 370 K to 540 K, with a typical uncertainty of less than 20 K. According to our data the temperature increases with latitude from the equator to the poles by 100–150 K. At similar latitudes, the temperature varies by 20–50 K at different times with no evidence for any systematic diurnal trend so far. Based on our data, the exobase of Saturn is 2700–3000 km above the 1 bar level and the thermal escape parameter near the exobase ranges from 260 to 340, implying that thermal escape from Saturn is firmly in the Jeans regime. The mixing ratio of H₂ is close to unity at all altitudes below the exobase. We find that the pressure levels in the thermosphere deviate significantly from a simple spheroid predicted by potential theory. This is consistent with significant meridional temperature variations in the lower thermosphere. A global analysis of the temperature structure at different depths in the atmosphere is required to constrain both the shape and the deposition and redistribution of energy in the upper atmosphere further.  相似文献   

Global photometric properties of Asteroid (4) Vesta observed with Dawn Framing Camera     

Jian-Yang Li  Lucille Le Corre  Stefan E. Schröder  Vishnu Reddy  Brett W. Denevi  Bonnie J. Buratti  Stefano Mottola  Martin Hoffmann  Pablo Gutierrez-Marques  Andreas Nathues  Christopher T. Russell  Carol A. Raymond 《Icarus》2013

Dawn spacecraft orbited Vesta for more than one year and collected a huge volume of multispectral, high-resolution data in the visible wavelengths with the Framing Camera. We present a detailed disk-integrated and disk-resolved photometric analysis using the Framing Camera images with the Minnaert model and the Hapke model, and report our results about the global photometric properties of Vesta. The photometric properties of Vesta show weak or no dependence on wavelengths, except for the albedo. At 554 nm, the global average geometric albedo of Vesta is 0.38 ± 0.04, and the Bond albedo range is 0.20 ± 0.02. The bolometric Bond albedo is 0.18 ± 0.01. The phase function of Vesta is similar to those of S-type asteroids. Vesta’s surface shows a single-peaked albedo distribution with a full-width-half-max ∼17% relative to the global average. This width is much smaller than the full range of albedos (from ∼0.55× to >2× global average) in localized bright and dark areas of a few tens of km in sizes, and is probably a consequence of significant regolith mixing on the global scale. Rheasilvia basin is ∼10% brighter than the global average. The phase reddening of Vesta measured from Dawn Framing Camera images is comparable or slightly stronger than that of Eros as measured by the Near Earth Asteroid Rendezvous mission, but weaker than previous measurements based on ground-based observations of Vesta and laboratory measurements of HED meteorites. The photometric behaviors of Vesta are best described by the Hapke model and the Akimov disk-function, when compared with the Minnaert model, Lommel–Seeliger model, and Lommel–Seeliger–Lambertian model. The traditional approach for photometric correction is validated for Vesta for >99% of its surface where reflectance is within ±30% of global average.  相似文献   

Integrating radar stratigraphy with high resolution visible stratigraphy of the north polar layered deposits,Mars     

S. Christian  J.W. Holt  S. Byrne  K.E. Fishbaugh 《Icarus》2013

Shallow Radar (SHARAD) on board NASA’s Mars Reconnaissance Orbiter has successfully detected tens of reflectors in the subsurface of the north polar layered deposits (NPLD) of Mars. Radar reflections are hypothesized to originate from the same material interfaces that result in visible layering. As a first step towards verifying this assumption, this study uses signal analyses and geometric comparisons to quantitatively examine the relationship between reflectors and visible layers exposed in an NPLD outcrop. To understand subsurface structures and reflector geometry, reflector surfaces have been gridded in three dimensions, taking into account the influence of surface slopes to obtain accurate subsurface geometries. These geometries reveal reflector dips that are consistent with optical layer slopes. Distance–elevation profiling of subsurface reflectors and visible layer boundaries reveals that reflectors and layers demonstrate similar topography, verifying that reflectors represent paleosurfaces of the deposit. Statistical and frequency-domain analyses of the separation distances between successive layers and successive reflectors confirms the agreement of radar reflector spacing with characteristic spacing of certain visible layers. Direct elevation comparisons between individual reflectors and discrete optical layers, while necessary for a one-to-one correlation, are complicated by variations in subsurface structure that exist between the outcrop and the SHARAD observations, as inferred from subsurface mapping. Although these complications have prevented a unique correlation, a genetic link between radar reflectors and visible layers has been confirmed, validating the assumption that radar reflectors can be used as geometric proxies for visible stratigraphy. Furthermore, the techniques for conducting a stratigraphic integration have been generalized and improved so that the integration can be undertaken at additional locations.  相似文献   

Lunar atmospheric H₂ detections by the LAMP UV spectrograph on the Lunar Reconnaissance Orbiter     

S. Alan Stern  Jason C. Cook  Jean -Yves Chaufray  Paul D. Feldman  G. Randall Gladstone  Kurt D. Retherford 《Icarus》2013

We report on the detection of H₂ as seen in our analysis of twilight observations of the lunar atmosphere observed by the LAMP instrument aboard NASA’s Lunar Reconnaissance Orbiter. Using a large amount of data collected on the lunar atmosphere between September 2009 and March 2013, we have detected and identified, the presence of H₂ in the native lunar atmosphere, for the first time. We derive a surface density for H₂ of 1.2 ± 0.4 × 10³ cm⁻³ at 120 K. This is about 10 times smaller than originally predicted, and several times smaller than previous upper limits from the Apollo era data.  相似文献