SHEBA flux–profile relationships in the stable atmospheric boundary layer

Measurements of atmospheric turbulence made during the Surface Heat Budget of the Arctic Ocean Experiment (SHEBA) are used to examine the profile stability functions of momentum, φ _m , and sensible heat, φ _h , in the stably stratified boundary layer over the Arctic pack ice. Turbulent fluxes and mean meteorological data that cover different surface conditions and a wide range of stability conditions were continuously measured and reported hourly at five levels on a 20-m main tower for 11 months. The comprehensive dataset collected during SHEBA allows studying φ _m and φ _h in detail and includes ample data for the very stable case. New parameterizations for φ _m (ζ) and φ _h (ζ) in stable conditions are proposed to describe the SHEBA data; these cover the entire range of the stability parameter ζ = z/L from neutral to very stable conditions, where L is the Obukhov length and z is the measurement height. In the limit of very strong stability, φ _m follows a ζ ^1/3 dependence, whereas φ _h initially increases with increasing ζ, reaches a maximum at ζ ≈ 10, and then tends to level off with increasing ζ. The effects of self-correlation, which occur in plots of φ _m and φ _h versus ζ, are reduced by using an independent bin-averaging method instead of conventional averaging.     

Landslide investigations in Russia and the former USSR

Landslide hazard has always been a focus of research of scientific and industrial organizations in Russia, as well as the former Soviet Union . This research included a broad spectrum of studies of landslide processes based on monitoring data collected at specialized stations nationwide, as well as the data collected and analyzed by various government and academic research institutions. The current study summarizes a vast body of knowledge encompassing an inventory of landslide cases, overview of mechanisms of landslide development and monitoring and slope stability assessments. It presents a new mechanism-based landslide classification and proposes a practical method of increasing slope resistance. Partial findings have been previously presented in numerous publications. We believe these findings have a worldwide significance and can be applied in different regions of our planet.     

Relaxation time distribution from time domain induced polarization measurements

We propose an algorithm for inverting time domain induced polarization data to a relaxation time distribution. The algorithm is based on the (Tikhonov) regularized solution of the 1^st kind Fredholm integral equation. We test the algorithm on synthetic data, and show its robustness for a noise level, typical of laboratory time domain measurements. We also show that, for the inversion purpose, the time domain data must be obtained with the different current wavelengths. We then test the algorithm on the experimental data recently obtained on brine-saturated medium-grained quartz sand (average grain diameter of 4 × 10⁻⁴ m), and on sand mixtures. For the medium-grained sand, relaxation time distribution contains a main peak at 25 s. Different amounts (3%, 8% and 12%) of fine-grained quartz sand (average grain diameter of 1.12 × 10⁻⁴ m) were added to the medium-grained quartz sand. For the sand mixture, an additional peak is observed in the relaxation time distributions, in the time range from 1.0 to 2.5 s. The magnitude of the second peak increases with the increase of the fine-grained sand content. Therefore, the experimental data show that peaks in the relaxation time distributions are related to the grain size. On the basis of the known peak location, and of the known grain size value, we obtained the values of the diffusion coefficient, which were found to be of the same order of magnitude as those in the bulk solution.     

3 Ma以来轨道尺度东亚冬季风演化的模拟研究

轨道尺度东亚冬季风变率对认识第四纪东亚环境演化和北半球冰盖演化具有重要的作用。文章利用德国波茨坦气候影响研究所的中等复杂程度地球系统模式(CLIMBER-2)对过去3 Ma气候和环境的模拟结果,探讨了轨道尺度东亚冬季风演化特征及其变化机制。采用两种指数反映东亚冬季风强度,分别指示中纬度西风强度(EAWMU)和东亚北风强度(EAWMV)。CLIMBER-2较好地模拟出了3 Ma以来地球冰期-间冰期旋回特征,以及第四纪以来全球变冷趋势。东亚冬季风在过去3 Ma以来呈现逐渐增强的趋势,EAWMV和EAWMU分别在约2.6 Ma和约1.5 Ma突然增强。EAWMV(EAWMU)在约2.2 Ma(约1.5 Ma)之前主要以20 ka岁差周期为主导,约2.2~1.0 Ma(约1.5~1.0 Ma)的转型期以41 ka倾角周期和20 ka岁差周期为主导,约1.0 Ma之后则均出现100 ka、41 ka和20 ka这3个轨道周期特征,并以100 ka偏心率周期为主导。在约2.2 Ma(约1.5 Ma)之前,EAWMV(EAWMU)主要受控于太阳辐射的直接强迫作用,北半球冰盖的作用相对较弱,在此之后北半球冰盖起主导作用,太阳辐射的直接强迫作用相对较弱。因此,第四纪东亚冬季风与北半球冰盖存在复杂的耦合关系,当冰盖规模较小时,它们的关系很弱;反之,当冰盖规模较大时,它们的联系加强。

     

Spectroscopic and photometric observations of symbiotic nova PU Vul during 2009–2016

A new set of low-resolution spectral and UBVJHKL-photometric observations of the symbiotic nova PU Vul is presented. The binary has been evolving after its symbiotic nova outburst in 1977 and now it is in the nebular stage. It is found that the third orbital cycle(after 1977) was characterized by great changes in associated light curves. Now, PU Vul exhibits a sine-wave shape in all the light curves(with an amplitude in the U band of about 0.7 mag), which is typical for symbiotic stars in the quiescent state. Brightness variability due to pulsations of the cool component is now clearly visible in the VRI light curves. The amplitude of the pulsations increases from 0.5 mag in the V band to 0.8 mag in the I band. These two types of variability, as well as a very slow change in the physical parameters of the hot component due to evolution after the outburst of 1977, influence the spectral energy distribution(SED)of the system. The variability of emission lines is highly complex. Only hydrogen line fluxes vary with orbital phase. An important feature of the third orbital cycle is the first emergence of the OVI, 6828  Raman scattering line. We determine the temperature of the hot component by means of the Zanstra method applied to the He II, 4686  line. Our estimate is about 150 000 K for the spectrum obtained near orbital maximum in 2014. The VO spectral index derived near pulsation minimum corresponds to M6 spectral class for the cool component of PU Vul.     

From Big to Little Rip in modified F(R,G) gravity

We discuss the cosmological reconstruction in modified Gauss-Bonnet (GB) gravity. It is demonstrated that the modified GB gravity may describe the most interesting features of late-time cosmology. We derive explicit form of effective phantom cosmological models ending by the finite-time future singularity (Big Rip) and without singularities in the future (Little Rip).