Frictional behavior during cold ring compression process of aluminum alloy 5052

The friction is the considerable boundary condition in bulk metal forming. In this paper, the ring compression test was used to evaluate the friction coefficient and factor in Coulomb friction model and Tresca friction model for the plastic deformation of aluminum alloy AA5052. The micro-macro analysis method combining surface morphology and micro-texture was used to explore the friction behaviors in AA5052 cold forming process. In general, the magnitude (μ or m) of friction changes before and after a deformation threshold during ring compression. The maximum change rate of the magnitude (μ or m) before and after the deformation threshold is close to 18.5% under the present experimental conditions, and the change rate decreases with increasing loading speed. The lubrication using MoS₂ is better than that using oil at lower speeds (0.15 mm/s, 1.5 mm/s), but the lubrications for MoS₂ and oil are similar at higher speeds (15 mm/s). The surface roughness, three-dimensional topography, and surface texture of compressed ring have a sudden change around the deformation threshold, which deviate from the previous evolution trend. The increased friction after deformation threshold also promotes the formation of sufficient shear strain layer in the subsurface plane of the compressed ring, and then it hinders the formation of the typical deformation textures with β-oriented line and promotes the appearance of shear textures such as $\left\{\text{001}\right\}〈\text{110}〉$, $\left\{\text{111}\right\}〈\mathit{uvw}〉$ and $\left\{\mathit{hkl}\right\}〈110〉$ textures.     

基于隐式温度修正的二维热线风速仪校准方法

热线风速仪主要用于湍流流场测量。热线测量的主要误差来源是由环境温度变化导致的热线校准参数的变化。Brunn提出的传统温度效应修正方法在环境温度变化较大的情况下会带来明显的误差。本文经过理论推导,提出了一种新的基于隐式温度修正的二维热线风速仪校准方法,并开展了热线校准实验研究。结果表明:当环境温度变化在4℃范围内时,本文提出的方法与Brunn方法的测量精度相当;当环境温度变化超过4℃时,本文提出的方法的测量精度远高于Brunn方法。     

Influences of milling and grinding on machined surface roughness and fatigue behavior of GH4169 superalloy workpieces

Surface topography of superalloy GH4169 workpieces machined by milling and grinding is different significantly. Meanwhile, surface roughness, as one of the main indicators of machined surface integrity, has a great influence on the fatigue behavior of workpieces. Based on analyzing the formation mechanism and characteristics of surface roughness utilizing different machining processes and parameters, the machined surface roughness curve can be decoupled into two parts utilizing frequency spectrum analysis, which are kinematic surface roughness curve and stochastic surface roughness curve. The kinematic surface roughness curve is influenced by machining process,parameters, geometry of the cutting tool or wheel, the maximum height of which is expressed as R'_z.By subtracting the kinematic part from the measurement curve, the stochastic surface roughness curve and its maximum height R'_zcan be obtained, which is influenced by the defects of cutting tool edge or abrasive grains, built-up edges(BUE), cracks, high frequency vibration and so on. On the other hand, the results of decoupling analysis of surface roughness curves indicate that Raand Rz values of milling GH4169 are 2–5 times and 1–3 times as high as those of grinding, while R'_zvalue of milling is 13.85%–37.7% as high as that of grinding. According to the results of fatigue life tests of specimens machined by milling and grinding, it can be concluded that fatigue behavior of GH4169 decreases with the increase of R'_zmonotonically, even utilizing different machining processes.     

Supersonic expansion on non-equilibrium plasmas

In the supersonic expansion of an ionized gas, the dominant factor in describing the atomic processes is the recombination rate constant K_R. Several models describing the recombination process have been reviewed in some detail. It has been found that, depending on the adopted definition, different models will yield different values of K_R for the same electron temperature and number density. A comparison of experimentally and theoretically derived values for K_R has to be done with great care, as in the majority of the experiments K_R is determined from the measured rate of disappearance of free electrons. These measurements give the correct “decay coefficient”, but only in certain circumstances will it reduce to the correct recombination rate. In the light of the important role that K_R plays in any numerical solution of nonequilibrium expansion flow of plasmas, details of experiments on a 15-degree corner expansion flow of ionized argon are given. In these experiments the plasma flow which was generated by driving strong normal shock waves into quiescent argon was studied mainly by optical diagnostics. Using a dual-frequency laser interferometer, the plasma properties around a corner expansion were recorded. The analysis of the interferograms has yielded values for the recombination rate constant as a function of the plasma macroscopic properties. The range of shock Mach number, electron number density, temperature and initial channel pressure and temperature were as follows:

$\text{13 < M, < 19; 10}{}^{16}\text{< n, < 1.5 × 10}{}^{17}\text{cm}{}^{\mathrm{?3}}\text{; 9000°}\text{K}\text{< T < 13,000°}\text{K}\text{; 2.2 < p}{}_1\text{< 10}\text{torr}\text{; T}{}_1\text{? 300°}\text{K}\text{.}$

It was found that the theoretically predicted values for the three-body, electron-ion-electron collisional recombination rate are in good agreement with those measured gasdynamically in a well-defined flow. The measured flow quantities substantiate a previous analysis based on the method of characteristics.     

Assessment of gas temperature fluctuations in the GTE combustion chamber exit section at generalizing experimental data on fuel combustion efficiency

It is suggested that gas composition at every point of the combustion chamber exit section be characterized by the temperature values T _i (“ideal” temperature) corresponding to the local values of the air-to-fuel coefficient α _i under complete fuel combustion (ν _comb ≈ 1). It is assumed that the values of T _i are distributed over the exit section area (gas mass) linearly and the values of T _imax and T _imin can be determined by the experimental data on the gas temperature fields in the combustion chambers. The distribution of temperatures T _i is used when it is necessary to generalize the experimental data on fuel combustion efficiency in GTE combustion chambers.     

油膜干涉测量翼型壁面摩阻低速风洞试验技术

油膜干涉试验可以定量测量得到模型壁面的摩擦应力,是开展摩阻特性研究的有力工具。通过对油膜干涉试验技术中的试验原理、试验方法、误差修正、数据结果分析等关键问题的研究,初步建立了试验系统,具备了开展模型壁面摩阻特性研究的试验能力。综合分析表面热膜试验结果与数值计算结果,在以模型弦长为特征长度,试验雷诺数 Re ＝1．3×106的条件下,翼型表面摩擦应力沿模型弦向的分布规律具有较好的一致性。     

改进的Qiu滑移因子模型用于离心压气机叶轮的参数研究

为适用于微型离心压气机叶轮的通流设计,对Qiu滑移因子模型加入了3个经验参数.首先对经验参数的求解方法及参数对于设计精度的影响进行了分析研究,发现其中经验参数c_r对于设计精度影响较大.其次在通流设计中应用改进的Qiu滑移因子模型辅助生成叶片,用计算流体动力学(CFD)研究了c_r所影响的模型滑移因子,与数值流场的出口平均滑移因子对比,得到了多种叶轮总体参数下c_r的最佳取值.发现虽然微型、大型离心压气机叶轮总体参数变化范围很大,但c_r的取值均以0.7左右为其最佳值.      

Reception of the NKL (Jim Creek) transmitter onboard GEOS-1

At the beginning of the GEOS lifetime, some attempts have been made for taking advantage of the passes over Alaska. GEOS was then commanded in a fixed mode and the corresponding telemetry data were recorded at the NASA stations. For two passes over Jim Creek (48°2N–121°9W) where a powerful VLF transmitter (f ₀ = 18.6 kHz) is located, GEOS was put in a specific mode in order to study the magnetospheric electromagnetic field in the vicinity of f ₀. The results of one pass (June 11, from 0755 UT) are presented here.During this pass, a strong enhancement of all the e.m. components at f ₀ has been observed for a specific period of time, when GEOS was very near to the exact conjugacy with NKL. The distance, as measured on the ground, over which the signal was above -6 dB from the maximum is of the order of 800 km. During the corresponding period of time (0740–0750 UT), the satellite altitude varied between 8000 and 6000 km. The magnetospheric region where the signal is strong appears to be structured, as if there were many ducts.Preliminary results concerning the polarization characteristics of the signal are presented. In the absence of precise measurements of these characteristics, the comparison between the electric and magnetic components of the received signal is not easy to interpret. An examination of the onboard computed correlograms (in the frequency range from f ₀ -0.6 kHz to f ₀ +3.3 kHz) shows that, for this pass, no VLF emissions were triggered by NKL, at the altitude of the satellite.     

Experimental technique for the investigation of artificially generated disturbances in planar laminar hypersonic boundary layers

A new experimental method to introduce artificially disturbances into flat plate boundary layers was studied in the Ludwieg-tube wind tunnel of the DLR in Göttingen at a free-stream Mach number of M₁ = 5. For the investigations, a 500 mm long and 20 mm thick flat plate model was used which spanned the test section 400 mm in width. As disturbance source a spark device flush mounted to the model surface close to its leading edge was utilized. The hot wire measurements of natural and forced disturbances in the boundary layer of the flat plate were conducted at different streamwise positions. The charge conditions of the wind tunnel used were almost constant at p_charge ≈ 5 bar and T_charge ≈ 393 K. This resulted in a unit Reynolds number of $\text{Re}{}_1\text{/l ≈ 6.74 1 10}{}^6\text{m}{}^{\mathrm{-1}}$ and a mass flow of ρ₁u₁ = 30.34 kg/m²s. To check the flow quality of the tunnel and the laminar characteristic of the boundary layer optically, Schlieren pictures were taken prior to each measurement campaign. The artificially inserted wave packets were successfully measured at different streamwise and spanwise locations downstream of the spark source. The main wave parameters, e.g. wave numbers and wave inclination angle were deduced from the measurements.     

Large-scale Bright Fronts in the Solar Corona: A?Review of?��EIT waves��

??EIT waves?? are large-scale coronal bright fronts (CBFs) that were first observed in 195 Å images obtained using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO). Commonly called ??EIT waves??, CBFs typically appear as diffuse fronts that propagate pseudo-radially across the solar disk at velocities of 100?C700 km?s^?1 with front widths of 50?C100 Mm. As their speed is greater than the quiet coronal sound speed (c _s ??200 km?s^?1) and comparable to the local Alfvén speed (v _A ??1000 km?s^?1), they were initially interpreted as fast-mode magnetoacoustic waves ( $v_{f}=(c_{s}^{2} + v_{A}^{2})^{1/2}$ ). Their propagation is now known to be modified by regions where the magnetosonic sound speed varies, such as active regions and coronal holes, but there is also evidence for stationary CBFs at coronal hole boundaries. The latter has led to the suggestion that they may be a manifestation of a processes such as Joule heating or magnetic reconnection, rather than a wave-related phenomena. While the general morphological and kinematic properties of CBFs and their association with coronal mass ejections have now been well described, there are many questions regarding their excitation and propagation. In particular, the theoretical interpretation of these enigmatic events as magnetohydrodynamic waves or due to changes in magnetic topology remains the topic of much debate.     

Oriented molybdenum disulfide-silica/hydrogenated nitrile butadiene rubber composites: Effects of nanosheets on mechanical and dielectric properties

A series of non-covalently functionalized molybdenum disulfide-silica (f-MoS₂-SiO₂) nanocomposites was prepared by an in-situ assembled method and used to fabricate the oriented molybdenum disulfide-SiO₂/Hydrogenated Nitrile Butadiene Rubber (f-MoS₂-SiO₂/HNBR) composites. The characterization results show the synergistic dispersion between the functionalized molybdenum disulfide (f-MoS₂) nanosheets and SiO₂ nanoparticles. The addition of f-MoS₂ nanosheets can improve the dispersion of fillers in the rubber matrix and weaken the filler network. The non-covalently functionalization improves the interface interaction between f-MoS₂ nanosheets and the rubber matrix. Furthermore, the tensile strength of f-MoS₂-SiO₂/HNBR is 65.9% higher than that of SiO₂/HNBR by adding 1.0wt% of f-MoS₂. At the same time, the dielectric constant of f-MoS₂-SiO₂/HNBR is increased by 23.7% compared to SiO₂/HNBR due to the micro-capacitor structure of parallel f-MoS₂ nanosheets in the rubber matrix. Our work provides new ideas for the development of high-performance elastomer materials.     

The Supermassive Black Hole—Galaxy Connection

The observed scaling relations imply that supermassive black holes (SMBH) and their host galaxies evolve together. Near-Eddington winds from the SMBH accretion discs explain many aspects of this connection. The wind Eddington factor \(\dot{m}\) should be in the range ～1–30. A factor \(\dot{m}\sim 1\) give black hole winds with velocities v～0.1c, observable in X-rays, just as seen in the most extreme ultrafast outflows (UFOs). Higher Eddington factors predict slower and less ionized winds, observable in the UV, as in BAL QSOs. In all cases the wind must shock against the host interstellar gas and it is plausible that these shocks should cool efficiently. There is detailed observational evidence for this in some UFOs. The wind sweeps up the interstellar gas into a thin shell and propels it outwards. For SMBH masses below a certain critical (M–σ) value, all these outflows eventually stall and fall back, as the Eddington thrust of the wind is too weak to drive the gas to large radii. But once the SMBH mass reaches the critical M–σ value the global character of the outflow changes completely. The wind shock is no longer efficiently cooled, and the resulting thermal expansion drives the interstellar gas far from the black hole, which is unlikely to grow significantly further. Simple estimates of the maximum stellar bulge mass M _b allowed by self-limited star formation show that the SMBH mass is typically about 10^?3 M _b at this point, in line with observation. The expansion-driven outflow reaches speeds v _out?1200 km?s^?1 and drives rates \(\dot{M}_{\mathrm{out}}\sim 4000~\mathrm {M}_{\odot }\,\mathrm{yr}^{-1}\) in cool (molecular) gas, giving a typical outflow mechanical energy L _mech?0.05L _Edd, where L _Edd is the Eddington luminosity of the central SMBH. This is again in line with observation. These massive outflows may be what makes galaxies become red and dead, and can have several other potentially observable effects. In particular they have the right properties to enrich the intergalactic gas with metals. Our current picture of SMBH-galaxy coevolution is still incomplete, as there is no predictive theory of how the hole accretes gas from its surroundings. Recent progress in understanding how large-scale discs of gas can partially cancel angular momentum and promote dynamical infall offers a possible way forward.     

Solar Wind Turbulence and the Role of Ion Instabilities

Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are: (i) weakness of collisional dissipation and (ii) presence of several characteristic space and time scales. In this paper we discuss observational properties of solar wind turbulence in a large range from the MHD to the electron scales. At MHD scales, within the inertial range, turbulence cascade of magnetic fluctuations develops mostly in the plane perpendicular to the mean field, with the Kolmogorov scaling $k_{\perp}^{-5/3}$ for the perpendicular cascade and $k_{\|}^{-2}$ for the parallel one. Solar wind turbulence is compressible in nature: density fluctuations at MHD scales have the Kolmogorov spectrum. Velocity fluctuations do not follow magnetic field ones: their spectrum is a power-law with a ?3/2 spectral index. Probability distribution functions of different plasma parameters are not Gaussian, indicating presence of intermittency. At the moment there is no global model taking into account all these observed properties of the inertial range. At ion scales, turbulent spectra have a break, compressibility increases and the density fluctuation spectrum has a local flattening. Around ion scales, magnetic spectra are variable and ion instabilities occur as a function of the local plasma parameters. Between ion and electron scales, a small scale turbulent cascade seems to be established. It is characterized by a well defined power-law spectrum in magnetic and density fluctuations with a spectral index close to ?2.8. Approaching electron scales, the fluctuations are no more self-similar: an exponential cut-off is usually observed (for time intervals without quasi-parallel whistlers) indicating an onset of dissipation. The small scale inertial range between ion and electron scales and the electron dissipation range can be together described by $\sim k_{\perp}^{-\alpha}\exp(-k_{\perp}\ell_{d})$ , with α?8/3 and the dissipation scale ? _d close to the electron Larmor radius ? _d ?ρ _e . The nature of this small scale cascade and a possible dissipation mechanism are still under debate.