电沉积参数对Cr2O3超疏水膜层表面形貌和润湿性的影响

采用电沉积法在碳钢片表面制备Cr₂O₃微纳膜层,并用硬脂酸对其进行表面修饰,降低其表面能。通过单因素法依次优化电流密度、铬酸浓度、极间距和电沉积时间,分析所得Cr₂O₃超疏水膜层的表面形貌和润湿性。当电流强度为4A、铬酸浓度为1.5 mol/L、极间距为5 mm及电沉积时间为1 h时,经硬脂酸修饰后Cr₂O₃膜层的超疏水性能优异,其静态接触角达到153.52°,且滚动角为2.17°。     

基于PCA结合污染物迁移模型的油气田开采影响环境的风险评估研究

为改善油气田开采过程中的环境,本文结合主成分分析法(Principal Component Analysis)与污染物迁移模型,对研究区的油气田开采过程中的污染物进行了分析,主要研究其在土壤中的迁移程度。本研究首先介绍了油气田开采产生污染物的研究背景与污染物种类,其次结合主成分分析法对污染物中的主要成分进行了筛选,最后构建污染物迁移模型,对污染物在土壤以及水体中的迁移进行了研究。结果表明,本文中的主要污染物为石油类、酸、氟离子、氯离子和COD(Chemical Oxygen Demand)、BOD(Biochemical oxygen demand),石油类所占比重最大,为23.63%;石油类污染物在黑钙土中的迁移最广,直至土层厚度为35cm,污染物浓度从18365 mg/kg降到0;石油类污染物在黑钙土中的迁移符合负指数规律;当酸液浓度在1%、2%、3%、4%时,氢离子在土壤中随深度的变化一致,土层厚度为20cm时,11%的酸液酸值高于低浓度土壤酸值,11%的酸液在快速淋滤状态下比缓慢淋滤快一步到达定值;氯离子和氟离子的迁移深度变化基本符合负指数变化规律;低浓度的污染物比高浓度的污染物更早达到定值;石油类污染物在土壤中的迁移能力较弱;本次研究实验值与模拟值基本一致,研究成果良好。石油类污染物在土壤中的迁移能力较弱,酸性污染物对土壤有一定影响。     

Hourglass magnetic field from a survey of current density profiles

Modeling the magnetic field in prestellar cores can serve as a useful tool for studying the initial conditions of star formation. The analytic hourglass model of Ewertowski and Basu (2013) provides a means to fit observed polarimetry measurements and extract useful information. The original model does not specify any radial distribution of the electric current density. Here, we perform a survey of possible centrally-peaked radial distributions of the current density, and numerically derive the full hourglass patterns. Since the vertical distribution is also specified in the original model, we can study the effect of different ratios of vertical to radial scale length on the overall hourglass pattern. Different values of this ratio may correspond to different formation scenarios for prestellar cores. We demonstrate the flexibility of our model and how it can be applied to a variety of magnetic field patterns.     

中国梯田撂荒程度及空间格局分异研究

在城镇化和工业化的驱动下,中国丘陵山区耕地逐渐被边际化,耕地撂荒范围也迅速从劣质的坡耕地延展至优质的梯田,大规模梯田撂荒将会引发一系列社会和生态效应,科学评估中国山区梯田的撂荒程度及空间分布将有助于有效地应对耕地撂荒问题。本文通过全国抽样调查的方式对中国梯田的撂荒程度进行了调查,利用获取的中国329个县的560份村问卷测算了中国梯田撂荒规模,并进一步分析了梯田撂荒空间分异特征及驱动因素。结果显示：(1)全国梯田撂荒现象分布广泛,发生梯田撂荒的村庄占总调查村庄的比例为54%,撂荒面积占梯田总面积的比例达到9.79%;(2)梯田撂荒程度呈现“南高北低”的特征,南方丘陵山区较为严重,尤以长江中下游地区为最;(3)梯田撂荒的主要因素可归结为农业劳动力外出务工、梯田耕作机械化程度、灌溉条件、耕作交通条件等。减缓梯田撂荒,应因区精准施策,提高梯田区机械化水平等措施具有普适性,针对质量较差的梯田,可有序“退耕”,对于质量较好的梯田,可采用调整种植结构、加强农业基础设施建设、鼓励流转与规模经营等方式。     

Magnetic remote sensing of Europa’s ocean tides

Recent analyses of Galileo magnetometer and gravity data justifies approximations that allow estimates of the magnetic fields generated by Europa’s ocean tides to be made even though some of the ocean parameters that would generally be required are unavailable. We show solutions for the magnetic fields generated by published estimates of ocean tides on Europa and provide simple scaling formulas that can be used to estimate the magnetic-field amplitudes for other choices for the ocean tidal state. Because of the distinguished spatial/temporal form of these fields, it is expected that Europa’s ocean tides can be inferred from remote magnetic sensing by an orbiter of sufficient duration.     

Differential rotation and meridional flow of Arcturus

The spectroscopic variability of Arcturus hints at cyclic activity cycle and differential rotation. This could provide a test of current theoretical models of solar and stellar dynamos. To examine the applicability of current models of the flux transport dynamo to Arcturus, we compute a mean‐field model for its internal rotation, meridional flow, and convective heat transport in the convective envelope. We then compare the conditions for dynamo action with those on the Sun. We find solar‐type surface rotation with about 1/10th of the shear found on the solar surface. The rotation rate increases monotonically with depth at all latitudes throughout the whole convection zone. In the lower part of the convection zone the horizontal shear vanishes and there is a strong radial gradient. The surface meridional flow has maximum speed of 170 m/s and is directed towards the equator at high and towards the poles at low latitudes. Turbulent magnetic diffusivity is of the order 10¹⁵–10¹⁶ cm²/s. The conditions on Arcturus are not favorable for a circulation‐dominated dynamo (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Modeling spatio‐temporal nonlocality in mean‐field dynamos

When scale separation in space or time is poor, the mean‐field α effect and turbulent diffusivity have to be replaced by integral kernels by which the dependence of the mean electromotive force on the mean magnetic field becomes nonlocal. Earlier work in computing these kernels using the test‐field method is now generalized to the case in which both spatial and temporal scale separations are poor. The approximate form of the kernel for isotropic stationary turbulence is such that it can be treated in a straightforward manner by solving a partial differential equation for the mean electromotive force. The resulting mean‐field equations are solved for oscillatory α –shear dynamos as well as α² dynamos with α linearly depending on position, which makes this dynamo oscillatory, too. In both cases, the critical values of the dynamo number is lowered due to spatio‐temporal nonlocality.When scale separation in space or time is poor, the mean‐field α effect and turbulent diffusivity have to be replaced by integral kernels by which the dependence of the mean electromotive force on the mean magnetic field becomes nonlocal. Earlier work in computing these kernels using the test‐field method is now generalized to the case in which both spatial and temporal scale separations are poor. The approximate form of the kernel for isotropic stationary turbulence is such that it can be treated in a straightforward manner by solving a partial differential equation for the mean electromotive force. The resulting mean‐field equations are solved for oscillatory α –shear dynamos as well as α² dynamos     

Horizontal flows concurrent with an X2.2 flare in the active region NOAA 11158

Horizontal proper motions were measured with local correlation tracking (LCT) techniques in active region NOAA 11158 on 2011 February 15 at a time when a major (X2.2) solar flare occurred. The measurements are based on continuum images and magnetograms of the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. The observed shear flows along the polarity inversion line were rather weak (a few 100 m s^–1). The counter‐streaming region shifted toward the north after the flare. A small circular area with flow speeds of up to 1.2 km s^–1 appeared after the flare near a region of rapid penumbral decay. The LCT signal in this region was provided by small‐scale photospheric brigthenings, which were associated with fast traveling moving magnetic features. Umbral strengthening and rapid penumbral decay was observed after the flare. Both phenomena were closely tied to kernels of white‐light flare emission. The white‐light flare only lasted for about 15 min and peaked 4 min earlier than the X‐ray flux. In comparison to other major flares, the X2.2 flare in active region NOAA 11158 only produced diminutive photospheric signatures (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Cyclic light and period variations of the UV Leonis system

Solutions of the new standard V‐light curves for the EA type binary UV Leo are obtained using the PHOEBE code (0.31a version). Absolute parameters of the stellar components were then determined, enabling them to be positioned on the absolute magnitude‐color (l.e. M_V vs. B – V) isochrones diagram, based on which the age of the system is estimated to be >4×10⁹ yr. Also times of minima data (“O – C curve”) have been analyzed. Apart from an almost sinusoidal variation with a period of 29.63 yr, which modulates the orbital period, and was attributed to a third body orbiting around the system, other cyclic variation in the orbital period and also brightness, with time scales of 24.25 and 22.77 yr were found, respectively. We associate this with a magnetic activity cycle newly reported here for UV Leo (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)