Dark energy,co-evolution of massive black holes with galaxies,and ASTROD-GW

The detection of low frequency band (100 nHz–100 mHz) and very low frequency band (300 pHz–100 nHz) gravitational waves (GWs) is important for exploration of the equation of state of dark energy and the co-evolution of massive black holes (MBHs) with galaxies. Most galaxies are believed to have a massive black hole in the galactic core. In the formation of these black holes, merging and accretion are the two main processes. Merging of massive black holes generate GWs which could be detected by space GW detectors and Pulsar Timing Arrays (PTAs) to cosmological distances. LISA (Laser-Interferometric Space Antenna) is most sensitive to the frequency band 1 mHz–100 mHz, ASTROD-GW (ASTROD [Astrodynamical Space Test of Relativity using Optical Devices] optimized for Gravitational Wave detection) is most sensitive to the frequency band 100 nHz–1 mHz and PTAs are most sensitive to the frequency band 300 pHz–100 nHz. In this paper, we discuss the sensitivities and outlooks of detection of GWs from binary massive black holes in these frequency bands with an emphasis on ASTROD-GW. The GWs generated by the inspirals, merging and subsequent ringdowns of binary black holes are standard sirens to the cosmological distance. Using GW observations, we discuss the methods for determining the equation of state of dark energy and for testing the co-evolution models of massive black holes. ASTROD-GW is an optimization of ASTROD to focus on the goal of detection of GWs. The mission orbits of the 3 spacecraft forming a nearly equilateral triangular array are chosen to be near the Sun-Earth Lagrange points L3, L4 and L5. The 3 spacecraft range interferometrically with one another with arm length about 260 million kilometers. With 52 times longer in arm length compared to that of LISA, the strain detection sensitivity is 52 times better toward larger wavelength. The scientific aim is focused for gravitational wave detection at low frequency. The science goals include detection of GWs from MBHs, and Extreme-Mass-Ratio Black Hole Inspirals (EMRI), and using these observations to find the evolution of the equation of state of dark energy and to explore the co-evolution of massive black holes with galaxies.     

文化认同与英语学习:基于非英语专业大学生的历时研究

通过问卷对三个年级557名非英语专业大学生的英美文化认同进行了调查研究,发现总体上这些大学生对英美文化的认同呈上升趋势;文化认同与他们的课外英语学习时间呈弱正相关,而与专业、年龄、英语学习年限呈弱负相关;文化认同与性别、家庭背景和外在动机开始呈正相关而后来却呈负相关,始学年龄则相反;文化认同与内在动机呈显著正相关,而与英语水平呈不显著的正相关。     

高校创业教育系统的构建——基于协同学视角

协同创新作为一种全新的教育理念,为高校教育教学改革,尤其是创业教育指明了方向。基于协同学理论和大学生创业教育体系相互关系,分析了高校创业教育中存在的突出问题,从理念、内容、组织和政策四个层面构建了创业教育的系统模型。     

基于物理知识约束的数据驱动式湍流模型修正及槽道湍流计算验证

对湍流摩擦阻力的精准预测是学术界和工业界普遍关心的重要问题，而数据驱动式的湍流模型修正方法对此显示出较大的潜力和前景。提出了一种基于物理知识约束的数据驱动式湍流模型修正方法，根据湍流摩擦阻力分解获得先验物理知识，在S-A湍流模型的生成项中引入非均匀分布的修正因子，以修正因子为设计变量，设定包含物理知识约束的目标函数，利用离散伴随方法求解目标函数与设计变量之间的梯度关系，通过高效率的迭代求解获得修正因子的分布。以槽道湍流为例，验证了包含物理知识约束的数据驱动式建模方法的优势，并分析了物理知识约束对湍流摩擦阻力预测精度的影响，结果表明引入物理知识约束可进一步提高湍流摩擦阻力的预测精度。     

新媒体时代下大学生思想政治教育载体的创新

互联网在全球范围内快速发展,各种新媒体技术如雨后春笋般不断涌现,给高校思想政治教育带来了极大挑战,同时也促使着大学生思想政治教育工作者就如何运用各种新媒体对大学生进行思想政治教育进行积极的探索,进一步增强大学生思想政治教育的实效性。     

Numerical simulation of time delay interferometry for a LISA-like mission with the simplification of having only one interferometer

In order to attain the requisite sensitivity for LISA, laser frequency noise must be suppressed below the secondary noises such as the optical path noise, acceleration noise etc. In a previous paper (Dhurandhar, S.V., Nayak, K.R., Vinet, J.-Y. Time delay interferometry for LISA with one arm dysfunctional. Class. Quantum Grav. 27, 135013, 2010), we have found a large family of second-generation analytic solutions of time delay interferometry with one arm dysfunctional, and we also estimated the laser noise due to residual time-delay semi-analytically from orbit perturbations due to Earth. Since other planets and solar-system bodies also perturb the orbits of LISA spacecraft and affect the time delay interferometry (TDI), we simulate the time delay numerically in this paper for all solutions with the generation number n ? 3. We have worked out a set of 3-year optimized mission orbits of LISA spacecraft starting at January 1, 2021 using the CGC2.7 ephemeris framework. We then use this numerical solution to calculate the residual optical path differences in the second-generation solutions of our previous paper, and compare with the semi-analytic error estimate. The accuracy of this calculation is better than 1 cm (or 30 ps). The maximum path length difference, for all configuration calculated, is below 1 m (3 ns). This is well below the limit under which the laser frequency noise is required to be suppressed. The numerical simulation in this paper can be applied to other space-borne interferometers for gravitational wave detection with the simplification of having only one interferometer.     

Optical/X-ray correlations as a signature of jet-disc coupling in the accreting black hole XTE J1118+480

We interpret the rapid correlated UV/optical/X-ray variability of XTE J1118+480 as a signature of the coupling between the X-ray corona and a jet emitting synchrotron radiation in the optical band. We propose a scenario in which the jet and the X-ray corona are fed by the same energy reservoir where large amounts of accretion power are stored before being channelled into either the jet or the high energy radiation. This time-dependent model reproduces the main features of the rapid multi-wavelength variability of XTE J1118+480. A strong requirement of the model is that the total jet power should be at least a few times larger than the observed X-ray luminosity, implying a radiative efficiency for the jet _j  3 × 10⁻³. This would be consistent with the overall low radiative efficiency of the source. We present independent arguments showing that the jet probably dominates the energetic output of all accreting black holes in the low-hard state.     

Time dependent accretion onto a black hole in a disk plus corona system

Hard X-ray lightcurves exhibit delays of 1 s with respect to the soft X-ray lightcurves when the microquasar GRS 1915+105 is in the state of frequent, regular outbursts. Such outbursts are supposed to be driven by the radiation pressure instability of the inner disk parts. The hard X-ray delays are then caused by the time needed for the adjustment of the corona to changing conditions in the underlying disk. We support this claim by the computation of the time evolution of the disk, including a non-stationary evaporation of the disk and mass exchange with the corona.     

Magnetohydrodynamics in solar and space physics

Because of its proximity, our Sun provides a unique opportunity to perform high resolution observations of its outer layers throughout the whole electromagnetic spectrum. We can also theoretically model most of the fascinating physical phenomena taking place on the Sun, as well as their impact on the solar system.     

加强英汉句法对比 养成英语句法意识

英汉两种语言分属不同的语系，也形成了各自的句法特征，在教学中应结合高职高专学生的学习状况，重点从句子的基本框架，句子展开手段，句子语序与句子成分的词性这4个方面来加强英汉句法对比，以帮助学生把握英语句法的基本特征，养成句法意识，输出合乎规范的英语句子，从而达到基本的交际目的和意图。