The Hβ and Hγ lines in the spectrum of V1057 Cyg

We present the equivalent widths of the Hβ and Hγ absorption lines in the spectrum of V1057 Cyg measured from 1978–1990 spectrograms. The mean equivalent widths of these lines decreased approximately twofold during 1978–1985 and somewhat increased during 1987–1990. Using published UBV photometry, we show that there has been a correlation between the Hβ equivalent width and the ?U-B? color since 1983, with ?W _λ(Hβ)? increasing with decreasing?U-B? Based on our spectroscopic and photometric observations in 1978–1990, we assume that V1057 Cyg has passed to a qualitatively new stage of its development after 1985.     

Long-term cyclicity of the Herbig Ae star BF Ori: Giant protocomets and accretion from a protoplanetary disk

Having analyzed the light curve for the Herbig Ae star BF Ori, we justify the hypothesis of a giant protocomet, GPC I BF Ori, with a period of 6.3 years and semimajor axis a = 10 ± 3 AU. Passing through periastron, such a giant protocomet partially breaks up. During each passage through periastron, the protocomet and the fragments that follow it supply dust to circumstellar space for a certain period of time. This hypothesis can account for the entire complex of observable phenomena of cyclic Algol-like activity in Herbig Ae/Be and T Tauri stars. Conditions in a protoplanetary disk after cocoon breakup are discussed. We adduce arguments for the absence of a dust disk and for the weak effect of objects other than comets on cyclic large-scale variability.     

DEM起伏纹理的视觉认知内涵与多变量消隐方法

地形是在内外营力的共同作用之下综合形成的,不同类型的地形具有不同的起伏形态特征,从全局或宏观的观测视角,可以视觉感知到这种地形起伏及其特征规律。纹理是众多物体表面呈现的有规律的线条组合,DEM作为地形的数据表达,不同地形类型区域的起伏形态具有纹理的显著表征。目前,对于DEM纹理研究主要是从DEM影像认知的角度出发,利用图像纹理的计算方法进行地形纹理对象描述和指标的提取,并基于获取的纹理对象进行区域地形特征分析和地貌类型的分类,在视觉上的反映存在不足。DEM起伏纹理作为一种基于某种观测视角和尺度的地形要素组合对象,首先需要对其进行系统的视觉认知,明确基于视觉认知的DEM起伏纹理构成要素和不同视觉变量控制的纹理要素组合结构,通过实现DEM起伏纹理的多维可视化建模,达到DEM数字地形建模的抽象与简化。基于此,本文以DEM地形起伏纹理为研究对象,对DEM起伏纹理进行视觉认知,明确DEM起伏纹理的涵义并建立提取方法,使用建立的方法实现了DEM起伏纹理的提取,取得了较好的提取效果。从视觉感知的机制出发,确定了决定视觉感知结果的视觉变量组合。确定了包含景深、长度和邻域等用于视觉综合的参数,设计建立了多变量的DEM起伏纹理消隐方法。最后设置视觉变量并使用该方法实现了DEM起伏纹理的消隐,消隐后DEM起伏纹理的数量分别降低了45.2%和53.2%,视觉上也取得了较理想的结果,具有一定的应用价值。     

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。     

顾及形变控制的小屏幕变比例尺交通路线图生成方法

用户在旅游或者室外运动中经常将路线图显示于移动设备上以方便规划路线。然而移动设备显示屏幕通常较小,若较大范围的地图通过等比例尺缩小在小屏幕显示,可能会导致清晰度和辨识度的降低,尤其对于地图中地物较为密集的区域。本文提出一种自动化生成变比例尺地图的方法,通过更加均匀化地图显示内容密度分布以改善地图概览清晰度。在该方法中,首先对密度分布进行估计,密度估计主要考虑地图上路线空间分布以及地标与注记显示空间,然后根据所得到的密度分布进行变比例尺转换,最终生成的变比例尺结果图,其大小取决于给定显示尺寸。相较于现有变比例尺转换方法,本文提出的方法可以考虑了地标与注记显示空间,同时又能有效控制地图变形以提高地图识别。实验结果表明,通过本方法生成变比例尺结果图对地图概览的清晰度有着显著提高,并且能够保持良好的地图识别度。     

Atmospheric and Oceanic Excitations to LOD Change on Quasi-biennial Tune Scales

We use wavelet transform to study the time series of the Earth's rotation rate (length-of-day, LOD), the axial components of atmospheric angular momentum (AAM) and oceanic angular momentum (OAM) in the period 1962-2005, and discuss the quasi-biennial oscillations (QBO) of LOD change. The results show that the QBO of LOD change varies remarkably in amplitude and phase. It was weak before 1978, then became much stronger and reached maximum values during the strong El Nino events in around 1983 and 1997. Results from analyzing the axial AAM indicate that the QBO signals in axial AAM are extremely consistent with the QBOs of LOD change. During 1963-2003, the QBO variance in the axial AAM can explain about 99.0% of that of the LOD, in other words, all QBO signals of LOD change are almost excited by the axial AAM, while the weak QBO signals of the axial OAM are quite different from those of the LOD and the axial AAM in both time-dependent characteristics and magnitudes. The combined effects of the axial AAM and OAM can explain about 99.1% of the variance of QBO in LOD change during this period.     

Possible variability of the magnetic field of T Tau

Using the Main Stellar Spectrograph of the 6-m Special Astrophysical Observatory telescope equipped with a polametric analyzer, we measured the longitudinal magnetic field component B_∥ for the T Tauri stars T Tau and AS 507 on January 16 and 18 and February 15, 2003. For both stars, we determined only the upper limits on B_∥ from photospheric lines: +15±30 G for T Tau and ?70±90 G for AS 507. The magnetic field of AS 507 was not measured previously, while B_∥ for T Tau is lower than its values that we obtained in 1996 and 2002 (B_∥?150±50G), suggesting that the longitudinal magnetic field component in the photosphere of T Tau is variable. We also measured the longitudinal magnetic field component for T Tau in the formation region of the He I 5876 Å emission line. We found B_∥ in this region to be ?+650, ?+350, and ?+1100 G on January 16, 18, and February 15, 2003, respectively. Our observations on January 18 and February 15 correspond to virtually the same phase of the star's rotation period, but the profiles of the He I 5876 Å line differ markedly on these two nights. Therefore, we believe that the threefold difference between the B_∥ values on these nights does not result from observational errors. We discuss the possible causes of the B_∥ variability in the photosphere and the magnetosphere of T Tau.     

Photometric elements,apsidal motion,and a third body in the eclipsing binary HP Aur

Highly accurate W BV R photometric measurements of the eclipsing binary HP Aur were performed in 2002–2003 with the 48-cm AZT-14 reflector at the Tien-Shan High-Altitude Observatory to determine the rate of apsidal motion. A consistent system of physical and geometrical parameters of the components and the binary as a whole has been constructed for the first time by analyzing these new measurements together with other published data: we determined their radii (R₁ = 1.05R_⊙, R₂ = 0.82R_⊙) and luminosities (L₁ = 1.10L_⊙, L₂ = 0.46L_⊙), spectral types (G2V + G8V) and surface gravities (log g₁ = 4.38, log g₂ = 4.51), age (t = 9.5 × 10⁹ yr), and the distance to the binary (d = 197 pc). We detected an ultraviolet excess in the spectra of both components, \(\Delta (W - B) \simeq - 0\mathop .\limits^m 25\), that is probably attributable to a metal deficiency in the atmospheres of these stars. In this system of two solar-type stars, we found a third body with the mass M₃ sin i ₃ ³ = 0.17_M⊙ that revolved with the period P₃ = 13.7 yr around the eclipsing binary in a highly eccentric elliptical orbit: e₃ = 0.70 and A₃ sin i₃ ? 7 AU. The orbit of the eclipsing binary itself was shown to be also elliptical, but with a low eccentricity (e = 0.0025(5)), while apsidal motion with a period U_obs > 80 yr was observed at a theoretically expected period U_th ≈ 92 yr. At least 20 to 30 more years of photoelectric measurements of this star will be required to reliably determine U_obs.     

A long-term UBVRI photometric study of the pre-main sequence star V350 Cep

Results from UBVRI optical photometric observations of the pre-main sequence star V350 Cep during the period 2004-2014 are presented.The star was discovered in 1977 due to its remarkable increase in brightness by more than 5 mag(R).In previous studies,V350 Cep was considered to be a potential FUor or EXor eruptive variable.Our data suggest that during the period of observations the star maintains its maximum brightness with low amplitude photometric variations.Our conclusion is that V350 Cep was probably an intermediate object between FUors and EXors,similar to V1647 0ri.