A search for propylene oxide and glycine in Sagittarius B2 (LMH) and Orion

We have used the Mopra Telescope to search for glycine and the simple chiral molecule propylene oxide in the Sgr B2 (LMH) and Orion KL, in the 3-mm band. We have not detected either species, but have been able to put sensitive upper limits on the abundances of both molecules. The 3σ upper limits derived for glycine conformer I are  3.7 × 10¹⁴ cm⁻²  in both Orion-KL and Sgr B2 (LMH), comparable to the reported detections of conformer I by Kuan et al. However, as our values are 3σ upper limits rather than detections we conclude that this weighs against confirming the detection of Kuan et al. We find upper limits for the glycine II column density of  7.7 × 10¹² cm⁻²  in both Orion-KL and Sgr B2 (LMH), in agreement with the results of Combes et al. The results presented here show that glycine conformer II is not present in the extended gas at the levels detected by Kuan et al. for conformer I. Our ATCA results have ruled out the detection of glycine (both conformers I and II) in the compact hot core of the LMH at the levels reported, so we conclude that it is unlikely that Kuan et al. have detected glycine in either Sgr B2 or Orion-KL. We find upper limits for propylene oxide abundance of  3.0 × 10¹⁴ cm⁻²  in Orion-KL and  6.7 × 10¹⁴ cm⁻²  in Sgr B2 (LMH). We have detected fourteen features in Sgr B2 and four features in Orion-KL which have not previously been reported in the interstellar medium, but have not been able to plausibly assign these transitions to any carrier.     

Periodic nulls in the pulsar B1133+16

Numerous studies of the brightest Cambridge pulsar, B1133+16, have revealed little order in its individual pulses, apart from a weak 30-odd-rotation-period fluctuation feature and that some 15 per cent of the star's pulsars are 'nulls'. New Arecibo observations confirm this fluctuation feature and that it modulates all the emission, not simply the 'saddle' region. By replacing each pulse with a scaled version of the average profile, we were able to quench all subpulse modulation and thereby demonstrate that the star's 'null' pulses exhibit a similar periodicity. A subbeam carousel model with a sparse and irregular 'beamlet' population appears to be compatible with these characteristics.     

Hydrological modelling using data from monthly GCMs in a regional catchment

This study demonstrates the use of spatially downscaled, monthly general circulation model (GCM) rainfall and temperature data to drive the established HyMOD hydrological model to evaluate the prospective effects of climate change on the fluvial run‐off of the River Derwent basin in the UK. The evaluation results of this monthly hydrological model using readily available, monthly GCM data are consistent with studies on nearby catchments employing high‐temporal resolution data, indicating that useful hydro‐climatic planning studies may be possible using standard datasets and modest computational resources. HyMOD was calibrated against 5 km² gridded UK Climate Projections dataset data and then driven using monthly spatially interpolated (~5 km²) outputs from Hadley Centre Coupled Model, version 3 and the Canadian Centre for Climate Modelling and Analysis for Intergovernmental Panel on Climate Change Special Report on Emissions Scenarios (IPCC‐SRES) A2a and B2a covering the 2020s, 2050s and 2080s. Results for both GCMs project a decrease in annual run‐off in both GCM models and scenarios with higher values in the summer/autumn months, whereas an increase in the later winter months. Both Hadley Centre Coupled Model, version 3 and the Canadian Centre for Climate Modelling and Analysis show higher ranges of uncertainty during the winter season with higher values of run‐off associated with December in all three simulation periods and two scenarios. A seasonal comparison of run‐off simulations shows that both GCMs give similar results in summer and autumn, whereas disparities due to GCM uncertainties are more conspicuous in winter and spring. In this study, both the GCMs under A2a scenario have demonstrated the high possibility of time shift in monthly average peak run‐offs in the Derwent River by 2080s in comparison with the early 21st century. Copyright © 2013 John Wiley & Sons, Ltd.     

Equilibrium trading of climate and weather risk and numerical simulation in a Markovian framework

We consider financial markets with agents exposed to external sources of risk caused, for example, by short-term climate events such as the South Pacific sea surface temperature anomalies widely known by the name El Nino. Since such risks cannot be hedged through investments on the capital market alone, we face a typical example of an incomplete financial market. In order to make this risk tradable, we use a financial market model in which an additional insurance asset provides another possibility of investment besides the usual capital market. Given one of the many possible market prices of risk, each agent can maximize his individual exponential utility from his income obtained from trading in the capital market, the additional security, and his risk-exposure function. Under the equilibrium market-clearing condition for the insurance security the market price of risk is uniquely determined by a backward stochastic differential equation. We translate these stochastic equations via the Feynman–Kac formalism into semi-linear parabolic partial differential equations. Numerical schemes are available by which these semilinear pde can be simulated. We choose two simple qualitatively interesting models to describe sea surface temperature, and with an ENSO risk exposed fisher and farmer and a climate risk neutral bank three model agents with simple risk exposure functions. By simulating the expected appreciation price of risk trading, the optimal utility of the agents as a function of temperature, and their optimal investment into the risk trading security we obtain first insight into the dynamics of such a market in simple situations.

基于Flex和.NET的B/S系统权限管理的设计与实现

RIA技术具有交互能力强、界面表现力丰富等特点,成为目前B/S系统的主要开发方式。而权限管理作为系统必不可少的组成部分,是系统稳定和数据安全的保障。介绍开发过程中使用的主要技术,阐述基于Flex和.NET技术开发的权限管理的设计方案和实现方法,并成功应用于工业总图共享服务系统中。实践证明,该权限管理设计方案具有灵活简便、安全性高、扩展性强和业务无关性等优点。     

基于动态阈值的HJ-1B图像云检测算法研究

针对环境与灾害监测预报小卫星星座1B星(HJ-1B)的传感器波段特征,通过对云检测阈值的年度波动性分析,提出了一种基于波谱标准差异常的“动态阈值云检测算法”.该算法的实现主要是采用图像配准、波段运算、线性回归和误差分析等方法,获取云异常区域,进而剔除图像中的云像元.研究结果表明,该算法可以很好地检测出不同时相、不同类型下垫面上空的云像元,为有效利用HJ-1B数据并提高其图像分类精度发挥作用.     

基于最大似然法和SVM法的太湖流域HJ-1B影像分类

以太湖流域作为研究对象,基于环境减灾卫星HJ-1B影像数据,比较利用最大似然法和支持向量机法进行土地利用/覆盖分类的效果。结果显示,SVM法在总体分类精度和Kappa系数上较传统最大似然法有所提高。SVM分类方法对于有限样本的分类表现出优越的性能,改善了传统分类方法的局限性,具有很大的应用潜力。     

TRMM3B42降水产品在鄱阳湖流域梅川江子流域的精度评价(英文)

在鄱阳湖流域的梅川江子流域,利用52个站点9年(2001-2005及2007-2010)的日降水数据对V6和V7两个版本的TRMM 3B42降水产品进行了精度评价。该评价针对多个时空尺度进行,包括栅格和流域两个空间尺度,日、月和年三个时间尺度。为避免尺度不匹配问题,本文利用泰森多边形方法将点尺度的站点观测数据转换到与TRMM数据相同的栅格尺度。评价结果表明,V6和V7两个版本的TRMM3B42降水产品差别较小,整体上均轻微高估了降水量(偏差均为0.04)。在日尺度,栅格和流域空间尺度上V6和V7TRMM3B42降水产品的精度均较差,相对均方根误差在135%-199%之间。因此,在该地区利用3B42数据进行日尺度的水文分析前需要对其进行校正。在月和年尺度,栅格和流域两个空间尺度上V6和V7两个版本的TRMM 3B42降水产品精度均较高,决定系数达到0.91-0.99,相对均方根误差在4%-23%之间。这表明TRMM 3B42降水产品在该地区月和年尺度的水文分析方面具有很好的应用前景。     

X-ray observations of PSR B1259−63 near the 2007 periastron passage

PSR B1259−63 is a 48-ms radio pulsar in a highly eccentric 3.4-yr orbit with a Be star SS 2883. Unpulsed γ-ray, X-ray and radio emission components are observed from the binary system. It is likely that the collision of the pulsar wind with the anisotropic wind of the Be star plays a crucial role in the generation of the observed non-thermal emission. The 2007 periastron passage was observed in unprecedented details with Suzaku , Swift , XMM–Newton and Chandra missions. We present here the results of this campaign and compare them with previous observations. With these data we are able, for the first time, to study the details of the spectral evolution of the source over a 2-month period of the passage of the pulsar close to the Be star. New data confirm the pre-periastron spectral hardening, with the photon index reaching a value smaller than 1.5, observed during a local flux minimum. If the observed X-ray emission is due to the inverse Compton (IC) losses of the 10-MeV electrons, then such a hard spectrum can be a result of Coulomb losses, or can be related to the existence of the low-energy cut-off in the electron spectrum. Alternatively, if the X-ray emission is a synchrotron emission of very high-energy electrons, the observed hard spectrum can be explained if the high-energy electrons are cooled by IC emission in Klein–Nishina regime. Unfortunately, the lack of simultaneous data in the TeV energy band prevents us from making a definite conclusion on the nature of the observed spectral hardening and, therefore, on the origin of the X-ray emission.