利用一种自动识别算法移除天气雷达反射率因子中的亮带   总被引：2，自引：5，他引：2       下载免费PDF全文

陈明轩  高峰 《应用气象学报》2006,17(2):207-214

该文介绍了一种自动识别和移除雷达反射率因子资料中亮带的算法, 并对该算法进行了初步测试。该算法利用的是插值到直角坐标系中的雷达反射率因子资料, 其配置和运行也相对简单, 但却对移除亮带比较有效。首先, 设定一套雷达反射率因子垂直廓线的理想模板, 这些理想的模板能够在最大程度上反映不同亮带存在区域的雷达实际反射率因子的垂直廓线特征。然后, 在水平方向每个点上, 进行理想模板和实际反射率因子垂直廓线在垂直和水平两个方向上的拟合和差异计算, 来自动识别雷达反射率因子中存在的连续亮带区域。最后, 利用亮带之上和亮带之下的反射率因子值对亮带中的反射率因子值进行插值纠正, 就可以移除亮带。利用位于天津塘沽的我国新一代天气雷达 (CINRAD/SA) 的反射率因子资料, 通过个例分析和准业务运行试验, 均表明这个简单算法可以识别和移除绝大多数影响雷达定量降水估计的反射率因子亮带区域, 但是实际雷暴区域的反射率因子特征受到该算法的影响比较小。计算分析还表明, 在京津地区的初夏, 上述亮带区域一般容易出现在2.5 km左右的高度处。  相似文献   

Differences Between Mode I and Mode II Crack Propagation     

K. B. Broberg 《Pure and Applied Geophysics》2006,163(9):1867-1879

Although mode I and mode II crack propagation show many similarities, in particular when analysed by linear elastic fracture mechanics, they differ significantly in the micro-structural behaviour. These differences, which are clearly noticeable in the fracture surface morphology, lead to fundamental differences in the macroscopic behaviour. Thus, mode II crack expansion under remote loading, appears to obey micro-structural scaling laws, implying that the dimensions of the process region stay essentially constant during crack expansion, rather than increasing with crack length. Therefore, expanding mode II cracks can almost reach the Rayleigh velocity, and actually also intersonic velocities. An expanding mode I crack, on the other hand, seems to obey continuum scaling laws, implying that the dimensions of the process region increase in proportion to crack length, leading to self-similar crack expansion at a velocity significantly below the Rayleigh speed and dependent on the remote load.  相似文献   

基于无抽样小波的遥感影像薄云检测与去除   总被引：1，自引：0，他引：1  

陈奋  闫冬梅  赵忠明 《武汉大学学报(信息科学版)》2007,32(1):71-74

针对全色波段遥感影像提出了一种基于无抽样小渡变换的薄云去除算法。对实际的卫星影像和航空影像所进行的试验结果表明，该方法是十分有效的。  相似文献   

EGM96/2008重力场模型在似大地水准面构建中的应用     

王鸣鹤  孙成志  许丹萍  吴晓倩 《北京测绘》2020,(5):687-690

似大地水准面的构建可以将GPS测量的高程迅速转化为正常高,极大降低高程测量的成本,提高相关工作效率。将EGM96/2008重力场模型与“移去-恢复”法相结合,在矿区内建立似大地水准面,并使用不同的插值方法,验证最优方案。结果表明,使用二次线性插值的EGM2008重力场模型拟合效果更好,模型外符合精度达到3.6 mm,更适合应用于该区域似大地水准面构建。  相似文献   

The complex gravitational lens system B1933+503     

C. M. Sykes  I. W. A. Browne  N. J. Jackson  D. R. Marlow  S. Nair  P. N. Wilkinson  R. D. Blandford  J. Cohen  C. D. Fassnacht  D. Hogg  T. J. Pearson  A. C. S. Readhead  D. S. Womble  S. T. Myers  A. G. de Bruyn  M. Bremer  G. K. Miley  & R. T. Schilizzi 《Monthly notices of the Royal Astronomical Society》1998,301(2):310-314

We report the discovery of the most complex arcsec-scale radio gravitational lens system yet known. B1933+503 was found during the course of the CLASS survey and MERLIN and VLA radio maps reveal up to 10 components. Four of these are compact and have flat spectra; the rest are more extended and have steep spectra. The background lensed object appears to consist of a flat-spectrum core (quadruply imaged) and two compact 'lobes' symmetrically disposed relative to the core. One of the lobes is quadruply imaged while the other is doubly imaged. An HST observation of the system with the WFPC2 shows a galaxy with an axial ratio of 0.5, but none of the images of the background object is detected. A redshift of 0.755 has been measured for the lens galaxy.  相似文献   

Studies of ultracompact H ii regions — II. High-resolution radio continuum and methanol maser survey     

A. J. Walsh    M. G. Burton    A. R. Hyland  & G. Robinson 《Monthly notices of the Royal Astronomical Society》1998,301(3):640-698

High spatial resolution radio continuum and 6.67-GHz methanol spectral line data are presented for methanol masers previously detected by Walsh et al. (1997). Methanol maser and/or radio continuum emission is found in 364 cases towards IRAS -selected regions. For those sources with methanol maser emission, relative positions have been obtained to an accuracy of typically 0.05 arcsec, with absolute positions accurate to around 1 arcsec. Maps of selected sources are provided. The intensity of the maser emission does not seem to depend on the presence of a continuum source. The coincidence of water and methanol maser positions in some regions suggests there is overlap in the requirements for methanol and water maser emission to be observable. However, there is a striking difference between the general proximity of methanol and water masers to both cometary and irregularly shaped ultracompact (UC) H  ii regions, indicating that, in other cases, there must be differing environments conducive to stimulating their emission. We show that the methanol maser is most likely present before an observable UC H  ii region is formed around a massive star and is quickly destroyed as the UC H  ii region evolves. There are 36 out of 97 maser sites that are linearly extended. The hypothesis that the maser emission is found in a circumstellar disc is not inconsistent with these 36 maser sites, but is unlikely. It cannot, however, account for all other maser sites. An alternative model which uses shocks to create the masing spots can more readily reproduce the maser spot distributions.  相似文献   

Optical and near-infrared imaging of faint Gigahertz Peaked Spectrum sources     

I. A. G. Snellen    R. T. Schilizzi    M. N. Bremer    A. G. de Bruyn    G. K. Miley    H. J. A. Ro¨ttgering    R. G. McMahon  & I. Pérez Fournon 《Monthly notices of the Royal Astronomical Society》1998,301(4):985-1000

A sample of 47 faint Gigahertz Peaked Spectrum (GPS) radio sources selected from the Westerbork Northern Sky Survey (WENSS) has been imaged in the optical and near-infrared, resulting in an identification fraction of 87 per cent. The R  −  I R  −  K colours of the faint optical counterparts are as expected for passively evolving elliptical galaxies, assuming that they follow the R -band Hubble diagram as determined for radio-bright GPS galaxies. We find evidence that the radio spectral properties of the GPS quasars are different from those of GPS galaxies. The observed distribution of radio spectral peak frequencies for GPS sources optically identified with bright stellar objects (presumably quasars) is shifted compared with GPS sources identified with faint or extended optical objects (presumably galaxies), in the sense that a GPS quasar is likely to have a higher peak frequency than a GPS galaxy. This means that the true peak frequency distribution is different for the GPS galaxies and quasars, because the sample selection effects are independent of optical identification. The correlation between peak frequency and redshift that has been suggested for bright sources has not been found in this sample; no correlation exists between R magnitude (and therefore redshift) and peak frequency for the GPS galaxies. We therefore believe that the claimed correlation is actually caused by the dependence of the peak frequency on optical host, because the GPS galaxies are generally at lower redshifts than the quasars. The difference in the peak frequency distributions of the GPS galaxies and quasars is further evidence against the hypothesis that they form a single class of object.  相似文献   

A 408-MHz variability study of two fields in the region 6^h30^m, +45°     

J. M. Riley  & D. A. Green 《Monthly notices of the Royal Astronomical Society》1998,301(1):203-209

Variability in 408-MHz flux density, over a 1-yr interval between 1995 and 1996, has been investigated using the DRAO Synthesis Telescope for a complete sample of 322 sources with S _408 MHz > 80 mJy at galactic latitude b  = 15°; four sources are found to show significant flux density variations. These results, taken with those from a similar study at b  = 58°, indicate that 408-MHz variability over a time-scale of 1 yr is more uncommon than has previously been thought; variations at a level >10 per cent could have been detected in a statistically complete sample of about 150 of these sources and none was found. Variability over a period of 18 yr has also been investigated by comparing the DRAO data with those from the B3 catalogue for 182 sources with S _408 MHz > 200 mJy; five variables are found. Large flux density variations over a period of 18 yr are much more common than over 1 yr, with roughly one source in 15 showing variations at the 15 per cent level or greater. The statistics are not good enough to show any conclusive evidence for a dependence of variability on galactic latitude. Roughly half of the variable sources have spectra that are steep at high frequencies and flatten at low frequencies; the other half have flat radio spectra over the entire frequency range. Simultaneous observations at 1420 MHz, also with the DRAO Synthesis Telescope, have been used to investigate variability at this frequency as well, and indicate that over a period of 1 yr roughly half of the flat-spectrum sources vary at the 5 per cent level or greater.  相似文献   

Interferometer phase calibration sources — II. The region 0° ≤ δ_B1950≤ +20°     

Browne  Patnaik  Wilkinson  & Wrobel 《Monthly notices of the Royal Astronomical Society》1998,293(3):257-287

We present a catalogue of 781 compact radio sources in the declination range 0° ≤ δ_B1950≤ +20° whose positions have been measured to an rms accuracy of about 14 mas with the Very Large Array (VLA). These sources are primarily intended for use as phase calibration sources for the Jodrell Bank MERLIN. However, they will also be suitable as phase calibrators for the VLA and can be considered as candidate phase calibrators for very long-baseline interferometry (VLBI) networks.  相似文献   

Red quasars not so dusty     

C. R.Benn  M.Vigotti  R.Carballo  J. I.Gonzalez-Serrano  S. F.SÃ&#;¡nchez 《Monthly notices of the Royal Astronomical Society》1998,295(2):451-456

Webster et al. claimed that up to 80 per cent of QSOs may be obscured by dust. They inferred the presence of this dust from the remarkably broad range of B − K optical–infrared colours of a sample of flat-spectrum PKS radio QSOs. If such dust is typical of QSOs, it will have rendered invisible most of those which would otherwise have been detected by optical surveys. We used the William Herschel Telescope on La Palma to obtain K infrared images of 54 B3 radio QSOs selected at low frequency (mainly steep-spectrum), and we find that although several have very red optical–infrared colours, most of these can be attributed to an excess of light in K rather than a dust-induced deficit in B. We present evidence that some of the infrared excess comes from the light of stars in the host galaxy (some, as previously suggested, comes from synchrotron radiation associated with flat-spectrum radio sources). The B − K colours of the B3 QSOs provide no evidence for a large reddened population. Either the Webster et al. QSOs are atypical in having such large extinctions, or their reddening is not due to dust; either way, the broad range of their B − K colours does not provide evidence that a large fraction of QSOs has been missed from optical surveys.  相似文献