First Light Curve Analysis of NSVS 8294044,V1023 Her,and V1397 Her Contact Binary Systems

The first photometric light curve investigation of the NSVS 8294044,V1023 Her,and V1397 Her binary systems is presented.We used ground-based observations for the NSVS 8294044 system and Transiting Exoplanet Survey Satellite data for V1023 Her and V1397 Her.The primary and secondary times of minima were extracted from al the data,and,by collecting the literature,a new ephemeris was computed for each system.Linear fits for the O-C diagrams were conducted using the Markov Chain Monte Carlo (MCMC) method.Light curve solutions were performed using the PHysics Of Eclipsing BinariEs Python code and the MCMC approach.The systems were found to be contact binary stars based on the fillout factor and mass ratio.V1023 Her showed the O’Connell effect and a cold starspot on the secondary component was required for the light curve solution.The absolute parameters of the system were estimated based on an empirical relationship between orbital period and mass.We presented a new T–M equation based on a sample of 428 contact binary systems and found that our three target systems were in good agreement with the fit.The positions of the systems were also depicted on the M–L,M–R,q–L_(ratio),and M_(tot)–J_(0)diagrams in the logarithmic scales.

具有多重随机干扰的NSV自适应鲁棒轨迹跟踪控制

针对具有随机噪声输入干扰、泊松随机波动干扰和控制输入饱和的近空间飞行器(near space vehicle, NSV)纵向轨迹控制模型,提出一种自适应鲁棒轨迹跟踪随机控制方案,实现对高度和速度参考信号的有效跟踪。对于外环轨迹控制,分别针对高度子系统和速度子系统,设计鲁棒随机控制器,通过数值计算方法对等效控制输入转化,得到内环姿态控制所需的姿态角参考信号。针对内环姿态控制问题,基于反步控制(backstepping control, BC)方法、动态面控制(dynamic surface control, DSC)技术和随机鲁棒控制方法,设计一种基于辅助系统的自适应鲁棒随机控制方案,实现随机干扰下的NSV姿态精确跟踪,衰减多重随机噪声干扰和参数不确定的影响,获得满意的鲁棒H∞控制性能。数值仿真进一步验证了所提方案的有效性。

基于改进L-M算法的NSV姿态系统模糊建模

为了使T-S模糊系统能够更有效、精确地对非线性系统进行建模,提出了一种用于T-S模糊系统训练的改进的全局收敛Levenberg-Marquardt(L-M)算法,并给出了相应迭代步骤和模糊系统的在线训练方案.该算法是在局部误差界条件下,结合信赖域方法,根据逼近效果实时调节步长,有效避免了Jacobi矩阵奇异,并加快了算法的收敛速率.然后,将该算法应用于T-S模糊系统的训练中,在线调整模糊系统中各线性多项式的参数及模糊隶属度函数的参数,从而使模糊系统不过分依赖于专家经验,并且提高其逼近速度和精度.最后,将该算法运用于NSV姿态系统的T-S模糊建模中.仿真结果表明:该算法可以很好地逼近NSV姿态系统;与标准的L-M算法相比,该算法在保证精度的同时明显提高了收敛速度.

NSVS 1908107, an EB-type eclipsing binary in the open cluster NGC 869

We present a time-series BV CCD photometry for an EB-type eclipsing binary NSVS 1908107, a member of the young open cluster NGC 869. The photometric solution was obtained by using the 2003 version of the Wilson-Devinney code. It reveals that the system is a semi-detached binary with the secondary component filling its Roche lobe. The mass ratio was determined to be 0.059±0.001. With the physical parameters of the cluster, the masses, radii and luminosities of the two components of NSVS 1908107 are estimated to be M1 = 10.34±2.29 M⊙, R1 = 4.65re±0.34 Rspectivel⊙, L1 = 8076 y. The results s±371 L = 2.40 how tha⊙and M2 = 0.61 t the secondary co±0.13M⊙, R2±0.17 R⊙, L2 = 1054±48 L⊙mponent could be a giant or subgiant star with the outer envelope being stripped.

NSVS 2569022:a peculiar binary among W UMa stars with extremely small mass ratios

Photometric observations of the W UMa binary NSVS 2569022 are presented. The light curve solution reveals that both components are of F spectral type （temperatures T1 = T2 = 6100 K）. NSVS 2569022 undergoes a total eclipse of W subtype and the mass ratio is well-determined. Its extremely small value of only 0.077 implies that the target will probably experience instability and a possible merger. This value ranks NSVS 2569022 in sixth place among binaries with the smallest mass ratio. Based on an empirical relation of ＂period - total mass＂ for low mass-ratio binaries, we estimate the global parameters of NSVS 2569022： masses M1 = 1.17 M⊙ and M2 = 0.09 M⊙; radii R1 = 1.19 R⊙ and R2 = 0.38 R⊙; luminosities L1 = 1.73 L⊙ and L2 = 0.17L⊙. An analysis of the characteristics of binaries with extremely low-mass ratios is made. NSVS 2569022 turns out to be a peculiar binary among W UMa stars with extremely small mass ratios due to its unexpectedly small fill-out factor of only 0.014 （slightly overcontact configuration）.

First time-resolved CCD photometry and time-series analysis of NSV 13601

We present the first results of a time-resolved CCD photometric and time-series analysis of NSV 13601,a variable star in the constellation Pegasus.The 14′′Schmidt-Cassegrain telescope of Maharaja Krishnakumarsinhji Bhavnagar University(MKBU)was used for observations.Analysis was performed both in VStar and Period04 software,and their results were compared.The main results are as follows:From data analysis,its has period^77.784 d(MKBU data V)(VStar),~77.632 d(MKBU data Ic)(VStar),~77.058 d(MKBU data V)(Period04)and^49.560 d(MKBU data Ic)(Period04).Its V and I mean magnitudes for MKBU data are 12.203(V)and 11.292(I)mag respectively.We confirm it to be a variable star.

Photometric observations and light curve solutions of the W UMa stars NSVS 2244206,NSVS 908513,CSS J004004.7+385531 and VSX J062624.4+570907

Photometric observations in Sloan 9＇ and i＇ bands of four W UMa stars, NSVS 2244206, NSVS 908513, CSS J004004.7＋385531 and VSX J062624.4＋570907, are presented. The light curve solutions reveal that all targets have overcontact configurations with fillout factors within 0.15-0.26. Their components are G-K spectral types and are almost in thermal contact. They are also relatively close in size and luminosity： the radius ratios r2/r1 are within 0.75-0.90; the luminosity ratios 12/11 are within 0.53-0.63. The results of the light curve solution of CSS J004004.7＋385531 imply the weak limb-darkening effect of its primary component and possible presence of additional absorbing features in the system.

A close-in substellar object orbiting the sd OB-type eclipsing-binary system NSVS 14256825

NSVS 14256825 is the second discovered sdOB+dM eclipsing-binary system with an orbital period of 2.65 h. This special binary was reported to contain circumbinary planets or brown dwarfs by using the timing method. However, different results were derived by different authors because of the insufficient coverage of eclipse timings. Since 2008, we have monitored this binary for about 10 yr using several telescopes and 84 new times of light minimum were obtained with high precision. It is found that the O-C curve has been increasing recently and it shows a cyclic variation with a period of 8.83 yr and an amplitude of 46.31 seconds. The cyclic change cannot be explained by magnetic activity cycles of the red dwarf component because the required energy is much larger than that radiated by this component in one whole period. This cyclic change detected in NSVS 14256825 could be explained by the light-travel time effect via the presence of a third body. The lowest mass of the third body is determined to be 14.15 Mjupwhich is in the transition range between planets and brown dwarfs. The substellar object is orbiting around this evolved binary at an orbital separation of around 3 AU with an eccentricity of 0.12. These results indicate that NSVS 14256825 is the first sdOB-type eclipsing binary consisting of a hierarchical substellar object.The detection of a close-in substellar companion to NSVS 14256825 will provide some insights on the formation and evolution of sdOB-type binaries and their companions.

NSVS 01286630:a detached binary with a close-in companion

New photometric observations of NS VS 01286630 were performed and two sets of fourcolor（B, V, Rc, Ic） light curves（LCs） were obtained. Using the 2013 version of the Wilson-Devinney（W-D） code, we analyzed these data. The photometric solutions reveal that NS VS 01286630 is an active detached eclipsing binary（EB） with a high orbital inclination（nearly 90°）. Remarkably, the temperature of the primary component（the hotter star） is higher than the secondary one, but the value of mass ratio q（M2/M1）for NS VS 0128663 is more than 1, which can be explained in that the surface of the secondary component of NSVS 01286630 is covered with big cool starspots. Based on our new CCD mid-eclipse times and the data published until now, variations in the mid-eclipse times were reanalyzed in detail using a weighted least-squares method. It is discovered that the（O-C） diagram of the system shows a cyclic oscillation with a period of 3.61 yr and an amplitude of 0.001 d. The cyclic variation may be caused by the light-travel time effect（LTTE） due to the presence of a third companion, whose mass we calculated as M3 sin（i3） =0.11 M（⊙）. The third body may affect the orbital evolution of the central binary system by transferring angular momentum.

Observations and light curve solutions of the W UMa binaries V796 Cep,V797 Cep,CSS J015341.9+381641 and NSVS 3853195

Photometric observations in Sloan g′and i′bands of four W UMa binaries, V796 Cep,V797 Cep, CSS J015341.9＋381641 and NSVS 3853195, are presented. Our observations showed that CSS J015404.1＋382805 and NSVS 3853195 are the same star. We determined the initial epochs T_0 of all targets and found improved values for the period of NSVS 3853195. The light curve solutions of our data revealed that the components of each target are almost the same in terms of mass, temperature,radius and luminosity. The stellar components are G and K spectral types and undergo partial eclipses.All systems have barely-overcontact configurations and can be classified as H subtype W UMa binaries.We established that the relation between the luminosity ratio l_2/l_1 and mass ratio q of our targets is approximately l_2/l_1 = q^（1.5）.

Polynomial networks based adaptive attitude tracking control for NSVs with input constraints and stochastic noises

This paper proposes a backstepping technique and Multi-dimensional Taylor Polynomial Networks(MTPN)based adaptive attitude tracking control strategy for Near Space Vehicles(NSVs)subjected to input constraints and stochastic input noises.Firstly,considering the control input has stochastic noises,and the attitude motion dynamical model of the NSVs is actually modeled as the Multi-Input Multi-Output(MIMO)stochastic nonlinear system form.Furthermore,the MTPN is used to estimate the unknown system uncertainties,and an auxiliary system is designed to compensate the influence of the saturation control input.Then,by using backstepping method and the output of the auxiliary system,a MTPN-based robust adaptive attitude control approach is proposed for the NSVs with saturation input nonlinearity,stochastic input noises,and system uncertainties.Stochastic Lyapunov stability theory is utilized to analysis the stability in the sense of probability of the entire closed-loop system.Additionally,by selecting appropriate parameters,the tracking errors will converge to a small neighborhood with a tunable radius.Finally,the numerical simulation results of the NSVs attitude motion show the satisfactory flight control performance under the proposed tracking control strategy.

轻体钢拳NSV

20世纪60年代末,已经被苏联军队装备了30年的12.7毫米口径DSh K重机枪逐渐开始被时代甩在身后,它笨重的抢身、龟速的机动性以及无法保证的远程射击精度让士兵们牢骚不断。在这个背景下,一款名为"NSV"的新型12.7毫米口径重机枪很快应运而生。这款新枪的名称由它的3个设计者的姓氏首字母组合而成,从1972年列装苏军开始,至今已经书写了四十多年的辉煌。

Light curve solutions of six eclipsing binaries at the lower limit of periods for W UMa stars

Photometric observations are presented in V and I bands of six eclipsing binaries at the lower limit of the orbital periods for W UMa stars. Three of them are newly discovered eclipsing systems. The light curve solutions reveal that all shortperiod targets are contact or overcontact binaries and six new binaries are added to the family of short-period systems with estimated parameters. Four binaries have com- ponents that are equal in size and a mass ratio near 1. The phase variability shown by the V-I colors of all targets may be explained by lower temperatures on their back surfaces than those on their side surfaces. Five systems exhibit the O＇Connell effect that can be modeled by cool spots on the side surfaces of their primary components. The light curves of V1067 Her in 2011 and 2012 are fitted by diametrically opposite spots. Applying the criteria for subdivision of W UMa stars to our targets leads to ambiguous results.

执行器故障下临近空间飞行器容错控制重构

临近空间飞行器飞行条件复杂、气动环境恶劣,极易导致飞行器舵面出现故障,容错控制是保证飞行器安全运行的关键,对此提出了一种基于观测器-控制器的有限时间高精度容错控制重构策略.首先,为提高容错控制的精确性,在故障影响下飞行器姿态模型基础上,设计了双层快速自适应滑模观测器,实现对包含故障、干扰等在内的综合干扰有限时间估计,避免了传统自适应增益的过估计,从而有效提高观测器估计精度;进一步基于观测器估计值设计容错控制器,获得故障影响下的期望控制力矩,实现飞行姿态的有限时间容错控制.其次,针对故障时气动舵面实际提供的控制力矩难以满足期望值的问题,引入推力矢量喷管作为补充执行器.考虑故障舵面特性,采用基于二次规划的最优控制分配策略,将期望力矩合理分配到气动舵面及矢量喷管上,通过矢量喷管补偿故障舵面力矩损失,实现执行器故障下控制重构.最后,通过数值仿真验证了所设计观测器的优越性,并验证了所提出容错控制重构策略的有效性.

考虑跟踪性能约束的近空间飞行器控制器设计

针对一类可变后掠角的近空间飞行器(NSV)指令跟踪问题,考虑其受到外界扰动及参数不确定的影响,同时考虑系统的跟踪性能约束及姿态角速度约束,提出了一种基于模糊系统的切换控制器设计方法,确保系统在扰动影响以及给定约束下能够对给定信号进行稳定跟踪。建立了包含未知扰动及不确定项的近空间飞行器非线性切换模型;通过设计模糊系统对系统所受的总干扰进行实时估计,并基于反步法进行了切换控制器设计,在控制器中对干扰进行补偿;通过公共Barrier Lyapunov方法对系统稳定性及动态性能进行了分析。数值仿真算例校验了所提出方法的有效性及优越性。

丙氧鸟苷诱导转单纯疱疹病毒胸苷激酶基因人肺腺癌细胞A549凋亡研究

目的 :观察丙氧鸟苷 (GCV)对A5 49-TK细胞的作用与诱导细胞凋亡的关系。方法 :A5 49-TK、A5 49两种细胞经 5 0 μmol/LGCV作用 3～ 5d后 ,用电镜、流式细胞仪、细胞凋亡原位检测法 (Tunel)观察细胞凋亡。结果 :电镜下发现A5 49-TK细胞有凋亡特征 :如凋亡小体、半月征、核浓缩 ,流式细胞仪发现A5 49-TK细胞有亚G0 G1峰 ,凋亡细胞占 12 2 1%± 1 6 6 % ,而A5 49细胞无G0 G1峰 ,凋亡细胞占 1 32 %±0 2 5 % ,两者比较P <0 0 1。Tunel表明A5 49-TK、A5 49两种细胞凋亡发生率分别为 16 %± 1 6 7% ,2 5 %±0 36 % ,两者比较P <0 0 1。结论 :GCV诱导A5

考虑执行器动态和输入受限的近空间飞行器鲁棒可重构跟踪控制

针对多变量、不稳定的近空间飞行器姿态系统,在系统存在参数不确定和外部干扰的情况下,并考虑执行器动态和输入受限,提出一种鲁棒可重构跟踪控制策略.首先,利用二阶滑模干扰观测器分别重构姿态、角速率回路的复合干扰;其次,采用鲁棒二阶滑模积分滤波器的反推(backstepping)方法避免了控制器设计中微分项膨胀问题,利用鲁棒项抵消重构误差对系统的影响,以实现姿态控制器设计.然后,在考虑执行器动态、输入受限及舵面卡死故障下,给出一种线性矩阵不等式的在线优化舵面分配算法,以实现飞行器的姿态角渐近跟踪期望的制导指令.最后,仿真结果表明所提出的方法具有良好的跟踪控制性能.