一种新型混合控制技术的振动台模型试验研究

本文提出了基底隔震和上部结构变刚度／阻尼半主动控制结合的一种新型混合控制型式,并且通过小型电磁振动台模型试验来研究其控制效能,为其今后更进一步理论和实验研究奠定基础。     

基于熵权-IOWGA算子的变权组合预测新方法

针对熵权法组合权重分配固定不变的问题,提出一种基于IOWGA算子的权重分配方法,建立基于熵权-IOWGA算子的变权组合模型。该方法以各单一模型的预测精度作为诱导值,按每一期诱导值的大小对单一模型进行有序赋权,并将其应用到变形数据分析中。实验表明,该方法赋权过程合理,模型预测精度更高,更加适用于变形分析预测过程。     

基于随机森林算法的地表温度鲁棒降尺度方法

陆地表面温度是描述区域或者全球范围内陆地表面与大气的相互作用和能量平衡最重要的环境参数之一。针对目前尚未有遥感卫星能够同时提供具有高时间和高空间分辨率的地表温度产品的问题,国内外学者发展了多种对低空间分辨率的地表温度进行降尺度的算法。然而,由于对地表温度解释变量和降尺度模型的选择往往具有区域局限性,导致了降尺度模型的泛化能力受到了一定的限制。本文首先评估了地表反射率、遥感光谱指数、地形因子、地表覆盖、经纬度以及基本状态变量6类环境参量与地表温度之间的相关关系,并在此基础上筛选出最佳解释变量;同时,结合在非线性回归问题上表现比较优秀的随机森林算法,建立了一种鲁棒性的基于随机森林算法地表温度降尺度模型（RRF）。本文选取了中国范围内具有代表性的11个地区作为主要研究区,将空间分辨率为1 km的MODIS地表温度产品降尺度至90 m。以北京市2个典型地表类型的子区域为代表研究区,通过与传统的基于归一化植被指数与地表温度相关关系的TsHARP模型,以及基于红波段和近红外波段以及地表高程作为尺度因子建立的简单Basic-RF模型的对比分析可得,RRF模型在2个子研究区降尺度结果均优于TsHARP模型和Basic-RF模型,其均方根误差分别为2.39 K和2.27 K。通过进一步对2个子研究区训练的RRF进行交叉验证,证明在一个研究区训练的RRF应用至另一研究区的降尺度时,RRF模型表现出了较好的鲁棒性,降尺度结果的均方根误差分别为2.56 K和2.44 K,精度误差相差仅为0.17 K。通过将RRF应用于中国范围内的多个研究区,结果表明利用少量训练数据构建的RRF模型适用于大范围的区域,地表温度降尺度结果都能取得较好的精度。     

一些概率方法在非概率数学问题中的应用

通过列举的一些试题，来说明如何构造随机变量或概率模型，并利用某些概率知识来得出一些似乎与概率无关的结论。这样可将数学各个层次的知识有机地联系到一起，从而给解题者提供新的解题思路。     

负顾客可服务的M/G/1休假排队系统

研究一类具有负顾客可服务的M/G/1休假排队系统,其中服务规则为后到先服务(LCFS),休假策略为空竭服务多重休假(ES,MV),负顾客也可以接受服务,正顾客也可以抵消负顾客,即正负顾客处在对等的位置上,抵消原则为抵消系统中正在接受服务的顾客(RCH).由补充变量法和状态转移方程的分析得到了稳态队长分布的广义概率母函数表达式.     

Variability of the Hα and Na I D line profiles in the spectrum of FU Ori

The variations of line profiles in the spectrum of FU Ori during several consecutive nights, from January 3 through January 8, 1999, have been traced for the first time in the entire history of studying this star. The variations of the Hα and Na I D line profiles are regular in pattern; at each time, the profiles of these lines were similar to a particular profile observed previously, suggesting that the phenomenon is periodic. We argue that the profile variations result from the axial rotation of the inner accretion-disk and disk-wind regions for which the temperature distribution and the wind-streamline orientation are not axisymmetric. The cause of the asymmetry could be the interaction of circumstellar matter with the stellar magnetic field if the magnetic axis is greatly inclined to the rotation axis. The possible binary nature of FU Ori seems a less likely cause of the asymmetry.     

The CLEAN method of spectral analysis and its application to the oscillations of the cataclysmic variable TT Arietis

We studied the one-dimensional spectral analysis CLEAN applied to time series with unequal intervals, tested it with simulated signal, and showed it to be also applicable to noisy series, only the quality of the spectrum is closely correlated with the noise intensity. Applying this method to photometric data of the cataclysmic variable TT Ari quasi-periodic oscillations with periods around 20 min are recovered.     

Pulsations and apsidal motion in the eclipsing variable system DI Herculis

In 2003–2008, highly accurate photoelectric and CCD observations of the close binary system DI Her were performed in the V band. The light curves of three primary and three secondary eclipses were constructed. These observations, along with the highly accurate photoelectric observations of other authors obtained in different years from 1963 to 1986, have confirmed the difference between the observed (1 _. ^o 3 ± 0 _. ^o 1/100 yr) and theoretical (4 _. ^o 3/100 yr) rates of apsidal motion. Our photometric data are indicative of a possible variability in the system with period P′ = 1.175 days and amplitude A′ = 0 _. ^m 011, which is probably related to the pulsations of one of the components. There may be a third body in the system that produces in-phase variations in the times of primary and secondary minima with a period of 10.5 yr and an amplitude of 1 _. ^m 5.     

An electronic version of volume I of the General Catalogue of Variable Stars with improved coordinates

We present a new electronic version of the first volume of the General Catalogue of Variable Stars (GCVS), fourth edition, which contains data on 10558 variable stars in Andromeda-Crux (the constellations are ordered in the Catalog according to the Latin alphabet). This version incorporates the name lists of variable stars from no. 67 to no. 76 for the same constellations. The main distinctive feature of the new version is that it provides improved equatorial J2000.0 coordinates for 10349 stars (including those for 4587 stars corrected for proper motions). These are based on identifications with positional catalogs using finding charts and on our new measurements. We searched for a number of stars on original plates from the plate collections of several observatories. The version also includes a file of remarks to the first GCVS volume and a preliminary version of the file of bibliographic references to the entire fourth edition of the GCVS. Apart from a complete update of the positional information, the new version incorporates all the other corrections that were found to be necessary after the first GCVS volume was published (1985).     

Ultraviolet spectrum of FU Ori and a “Compromise” model of the FUor

We have analyzed the Hubble Space Telescope spectrum of the young star FU Ori in the range 2300–3100 Å. The long-wavelength part of the spectrum is similar to the spectrum of a supergiant with T _eff ? 5000–6000 K, but the range of wavelengths shorter than ?2600 Å is dominated by radiation from a region with T _eff ? 9000 K. We discuss the possibility of explaining these peculiarities of the spectrum, the Al II] 2669.2 emission line profile, and the results of X-ray observations for FU Ori in terms of an accretion disk model whose thickness increases as the star is approached starting from distances ?10¹² cm. Near the star, the disk has the shape of a cone in which only the part of its surface on the far (from the observer) side is visible. The suggested model is a kind of a compromise between the models of a thin α-disk and a supergiant: basically, this is an accretion model, but it resembles a supergiant in observational manifestations. Numerous absorption lines originating in the disk wind are superimposed on the disk spectrum. The wind is a cold (T ? 5000 K), dense (N _e ? 10¹¹ cm^?3) gas. The number of wind absorption lines in the ultraviolet spectrum of FU Ori increases with decreasing wavelength. This causes a rapid decline in intensity in the short-wavelength part of the spectrum. As a result, the maximum temperature in the disk estimated from low-resolution IUE spectra has been underestimated.