Broadband X-ray spectrum of the intermediate polar V2400 Oph     

M. G. Revnivtsev  A. A. Lutovinov  B. F. Suleimanov  S. V. Molkov  R. A. Sunyaev 《Astronomy Letters》2004,30(11):772-778

We present the results of our analysis of the observations of the intermediate polar V2400 Oph by the INTEGRAL and RXTE observatories. We reconstructed the spectrum of the source over a wide (3–100 keV) energy range. The spectrum obtained can be fitted by a computed theoretical model of the post-shock emitting region with T_max～22 keV. As a result, we estimated the mass (0.59M_⊙) and radius (8.8×10⁸ cm) of the white dwarf in the system V2400 Oph.  相似文献   

An Approach to Improving the Retrieval Accuracy of Oceanic Constituents in Case Ⅱ Waters     

ZHANGTinglu FrankFell 《中国海洋大学学报(英文版)》2004,3(2):220-224

1　Introduction　At present ,theretrievalofoceanicconstituentsfromoceancolourmeasurementsinCaseⅡwatersisoneofthemajorchallengesinoceancolourstudy(IOCCG ,2 0 0 0 ) .TheconstituentspresentinCaseⅡwatersaregenerallydividedintothreetypes :chloro phyll (CHL) …  相似文献   

彩色图像的输入指标对层次再现的影响   总被引：1，自引：0，他引：1  

马桃林 《武汉大学学报(信息科学版)》2005,30(9):829-832,845

层次和细微层次是评价图像复制质量的重要指标。对两种常用平台式扫描仪的输入指标进行检测,通过分析和对比实验,研究了各指标的作用规律,并分析其对图像层次和细微层次的影响,对不同类型的彩色原稿的扫描指数的设置都具有一定的指导意义。  相似文献   

翡翠的矿物组成及其宝石学意义   总被引：1，自引：0，他引：1       下载免费PDF全文

徐志  陶专  解永顺 《地质找矿论丛》2005,20(1):35-39

翡翠的矿物组成是影响翡翠质量及其物理性质的最根本原因,同时玉石质量也受其结构、构造的影响.辉石类矿物是组成翡翠的主要矿物,次要矿物包括有长石族矿物和闪石族矿物,常见的副矿物有铬铁矿、绿泥石、褐铁矿等.矿物组成的复杂性直接导致了翡翠种类、颜色的多样性变化,同时也对透明度、光泽度、比重、硬度及工艺性能等产生影响.所以,翡翠的矿物组成是质量分级评价最根本的依据,具有很重要的宝石学意义.  相似文献   

Upper Cretaceous oceanic red beds in southern Tibet:Lithofacies,environments and colour origin   总被引：6，自引：0，他引：6  

Jansa Luba 《中国科学D辑(英文版)》2006,49(8):785-795

  相似文献   

Fire Danger Monitoring Using ERS-1 SAR Images in the Case of Northern Boreal Forests     

Brigitte Leblon  Eric Kasischke  Marty Alexander  Mark Doyle  Melissa Abbott 《Natural Hazards》2002,27(3):231-255

Research was carried out to assess the potential of imaging radar systems formonitoring forest fire danger. In Canada, daily forest fire danger ratings are generated by the Canadian ForestFire Danger Rating System (CFFDRS), based on estimates of fire weather indices (FWI) and measured foliar moisturecontent (FMC). To evaluate the potential of imaging radar, an experiment was conducted using test sitesconsisting of jack pine, black spruce and white spruce stands located in the MacKenzie river basin, NorthwestTerritories, Canada. Radar image intensity values from ERS-1 SAR imagery collected over these stands in 1994 werecompared to FWI indices and FMC data. FWI indices were calculated using data from local weather stations.Seasonal trends in radar backscatter (⁰) were shown to correlate with temperature and precipitation. Significant relationships were found between ⁰ and FWI codes and indices, particularly in thecase of the black spruce stands, with slow-drying fuels, like duff moisture code (DMC), drought code (DC), and build-upindex (BUI). Rates of changes in ⁰were related to rates of changes in FMC, particularly in the case ofthe jack pine stands for old FMC and in the case of white spruce stands for composite FMC.  相似文献   

地气测量在宣汉气田上的应用   总被引：11，自引：1，他引：10  

杨凤根  童纯菡 《矿物岩石》1998,18(3):99-105

本文首次将地气测量技术应用于油气田勘查及评价工作中;即对由遥感方法发现的环形构造等有利含油气局部构造通过地气测量进行地面解译工作,研究结果表明,地气测量能够反映地下逾４０００ｍ的深部构造形成的弱异常;地气异常出现在由遥感解译的环形构造的环状带之正上方,异常宽度略大于遥感所反映环状带宽度。  相似文献   

White dwarf masses in magnetic cataclysmic variables: multi-temperature fits to Ginga data     

Mark Cropper  Gavin Ramsay  & Kinwah Wu 《Monthly notices of the Royal Astronomical Society》1998,293(3):222-232

One method of obtaining the mass of the white dwarf in magnetic cataclysmic variables (mCVs) is through their hard X-ray spectra. However, previous mass estimates using this method give lower limits because the temperature of the plasma in the post-shock region (where the hard X-rays are emitted) is lower than the temperature of the shock itself. In AM Her systems, the additional cooling of the post-shock plasma by cyclotron emission will further lower the derived mass. Here we present estimates of the masses of the white dwarf in 13 mCVs derived using Ginga data and a model in which X-rays are emitted from a multi-temperature emission region with the appropriate temperature and density profile. We include in the model reflection from the surface of the white dwarf and a partially ionized absorber. We are able to achieve good fits to the data. We compare the derived masses with previous estimates and the masses for larger samples of isolated white dwarfs and those in CVs.  相似文献   

Echoes from an irradiated disc in GRO J1655–40     

Hynes  O''Brien  Keith Horne  Chen  & Haswell 《Monthly notices of the Royal Astronomical Society》1998,299(4):L37-L41

Oscillations observed in the light curve of Nova V1974 Cygni 1992 since the summer of 1994 have been interpreted as permanent superhumps. From simple calculations based on the tidal disc instability model of Osaki, and assuming that the accretion disc is the dominant optical source in the binary system, we predict that the nova will evolve to become an SU UMa system as its brightness declines from its present value by another 2–3 mag. Linear extrapolation of its current rate of fading (in magnitude units) puts the time of this phase transition within the next 2–4 yr. Alternatively, the brightness decline will stop before the nova reaches that level, and the system will continue to show permanent superhumps in its light curve. It will then be similar to two other old novae, V603 Aql and CP Pup, which still display the permanent superhump phenomenon 80 and 56 yr, respectively, after their eruptions. We suggest that non-magnetic novae with short orbital periods could be progenitors of permanent superhump systems.  相似文献   

On the asphericity of nova remnants caused by rotating white dwarf envelopes     

John M. Porter  O'Brien  & Mike F. Bode 《Monthly notices of the Royal Astronomical Society》1998,296(4):943-948

The effect of rotating white dwarf envelopes in determining the structure of nova shells is examined. This is achieved by numerical hydrodynamic simulations of the flows around a binary star system. In previous studies of remnant formation, this rotation has not been included.
It is found that the structures formed in the flow are more consistent with observations of nova shells than the previous theoretical studies. The shells produced by the nova become more prolate with increasing white dwarf envelope rotation. Hence the rotation of white dwarf envelopes must be included in any future discussion of remnant formation.
A possible method of identifying the dominant process by which mixing of accreted and white dwarf matter takes place is suggested.  相似文献