RUSLE applied in a GIS framework: Calculating the LS factor and deriving homogeneous patches for estimating soil loss

The RUSLE (Revised Universal Soil Loss Equation) is integrated within a GIS framework to calculate soil loss spatially. For this module, algorithms and procedures were developed to derive the slope length factor (L) and steepness factor (S) from a DEM, then integrated with the R, K, C, and P factors to develop homogeneous patches (sub‐units) within each field or river basin. Soil loss is determined for each patch within a study unit, and then combined to determine the fields' or river basin's average annual and total soil loss. Two case studies are presented. The first case study, in central Massachusetts, compares estimated soil loss values obtained for individual fields using the Idrisi RUSLE module to USDA‐NRCS RUSLE field data. While soil loss results were similar, the RUSLE module allows fields to be partitioned into more similar units than practical in the field. This permits detailed spatial analysis of soil‐loss patterns. The second case study compares soil‐loss estimates for a catchment in southwestern Flanders, Belgium. This model–model comparison contrasts the results from the RUSLE module to the WATEM model—a grid cell based model based on the USLE/RUSLE but conceptualized in a multi‐flow context. Results between the predicted soil losses utilizing the two different approaches are significantly correlated. However, estimated soil losses are consistently higher for the WATEM model. This likely reflects the differences between how the two models compute L as well as the contribution of ephemeral gullies and flow convergence which are incorporated in WATEM but not in RUSLE.     

LS I +61 303 as a potential neutrino source on the light of magic results

Very high energy γ-rays have recently been detected from the microquasar LS I +61 303 using the MAGIC telescope. A phenomenological study on the concomitant neutrinos that would be radiated if the γ-ray emission is hadronic in origin is herein presented. Neutrino oscillations are considered, and the expected number of events in a km-scale detector such as ICECUBE is computed under different assumptions including orbital periodicity and modulation, as well as different precision in the modeling of the detector. We argue that the upper limits already imposed on the neutrino emission of LS I +61 303 using AMANDA-II and the forthcoming measurements by ICECUBE may significantly constrain – in an independent and unbiased way – the γ-ray to neutrino flux ratio, and thus the possibility of a hadronic origin of the γ-rays. The viability of hadronic models based on wind–jet interactions in the LS +61 303 system after MAGIC measurements is discussed.     

LTS 回归与最小一乘法稳健性比较

探讨了可以抵抗回归数据中出现的X与Y空间的多个异常点稳健回归估计方法,介绍了最小一乘法与LTS估计,并利用MATLAB模拟数据,分析以LS,LTS和最小一乘法三种方法对三组模拟数据进行分析比较,表明LTS方法比其他两种的抗粗差效果要好,具有很强的稳健性。     

An optimality property of the integer least-squares estimator

A probabilistic justification is given for using the integer least-squares (LS) estimator. The class of admissible integer estimators is introduced and classical adjustment theory is extended by proving that the integer LS estimator is best in the sense of maximizing the probability of correct integer estimation. For global positioning system ambiguity resolution, this implies that the success rate of any other integer estimator of the carrier phase ambiguities will be smaller than or at the most equal to the ambiguity success rate of the integer LS estimator. The success rates of any one of these estimators may therefore be used to provide lower bounds for the LS success rate. This is particularly useful in case of the bootstrapped estimator. Received: 11 January 1999 / Accepted: 9 July 1999     

拟准观测的选取和真误差估值的“分群”现象

以往检验粗差有两类不同的方法,一类是假设检验,另一类是抗差估计。它们虽然有显著不同,但都是以最小二乘残差及其函数为研究对象的。文献［8,9］提出了以真误差为研究对象的拟准检定法。该方法通过附加拟准观测真误差的估值极小的条件,直接求解关于真误差的秩亏方程,然后依据真误差估值的分布特征判别和定位粗差。 　拟准检定法的关键是如何正确的选择拟准观测。本文总结了实践中选择拟准观测的原则和方法。选择拟准观测可采用初选与复选两步来实施。初选时将观测值分为4类：“0”类是按一定规则经过初步判断怀疑含粗差可能性很大的,不宜选为拟准检测;“1”类是依内部可靠性指标衡量,所处位置结构差的观测;“2”类与“0”相反,是依一定指标判断含粗差可能性较小的观测;“3”类是除上述三种特殊情况以外,余下的观测。这四类观测中,“2”类以及“3”类中指标值ui相对较小的部分观测可初选为拟准观测。复选是在初选后计算出真误差估值的基础上,选取真误差估值绝对值较小的为拟准观测。本文指出拟准观测的初选可以不唯一。 　利用许多统计学者曾多次讨论过的一个算例［6,11］,详细介绍了选择拟准观测的过程,并将有关结果与以往的结果进行比较,用拟准检定法一方面排除了4个异常观测的影响,另一方面充分利用了其余观测的信息,结果可能更合理一些。 　拟准观测选择适当时,真误差估值有明显的“分群”现象。结合算例,本文用图表的形式形象地分析了这种有趣的现象。在表中,异常的和正常的真误差估值的量值有显著的分界带,含粗差的或异常观测的真误差明显大于正常的;在图中,异常值“浮”在分布图的上部,而正常值则“沉”在下方。依此特性可直观地判定粗差的位置。     

Physical parameters of the O6.5V+B1V eclipsing binary system LS 1135

The 'All Sky Automated Survey' (ASAS) photometric observations of LS 1135, an O-type single-lined binary (SB1) system with an orbital period of 2.7 d, show that the system is also eclipsing performing a numerical model of this binary based on the Wilson–Devinney method. We obtained an orbital inclination     . With this value of the inclination, we deduced masses   M ₁∼ 30 ± 1 M_⊙  and   M ₂∼ 9 ± 1 M_⊙  , and radii   R ₁∼ 12 ± 1 R_⊙  and   R ₂∼ 5 ± 1 R_⊙  for primary and secondary components, respectively. Both the components are well inside their respective Roche lobes. Fixing the T _eff of the primary to the value corresponding to its spectral type (O6.5V), the T _eff obtained for the secondary component corresponds approximately to a spectral type of B1V. The mass ratio   M ₂/ M ₁∼ 0.3  is among the lowest known values for spectroscopic binaries with O-type components.     

抗差主成分估计及应用

本文基于抗差估计和主成分估计理论，提出一种新的估计－抗差主成分估计，推导了参数的抗差主成分解，并结合算例进行了试算。结果表明：抗差主成分估计不仅可以解除法方程系数降的病态，而且对于抑制观测粗差的影响也有显著功效。     

GPS非线性数据处理的同伦最小二乘模型

基于非线性同伦思想 ,提出了非线性最小二乘同伦方法 ,并推导出相应的GPS同伦非线性模型和算法。算例表明 ,对于精度较差的初始值 ,采用同伦非线性GPS伪距定位模型较线性最小二乘求解精度要好。     

GPS网平差的多元响应-非线性最小二乘模型及其解的最优化混合算法

在控制网中,用GPS测量,可以同时测得一个点的基线向量,在具有起算数据时可获得观测点的三维坐标等多个响应变量值,将这些响应变量包含的信息综合起来,可以得到参数的更精确的估计。本文针对GPS测量数据为多元响应数据的特点,建立了一个GPS网平差的多元响应-非线性最小二乘模型,针对该模型,结合拟牛顿法和信赖域算法建立了一个新非线性优化的混合算法,该算法具有全局收敛性和超线性收敛性。