Grinding temperature and energy ratio coefficient in MQL grinding of high-temperature nickel-base alloy by using different vegetable oils as base oil

Vegetable oil can be used as a base oil in minimal quantity of lubrication(MQL). This study compared the performances of MQL grinding by using castor oil, soybean oil, rapeseed oil, corn oil, sunflower oil, peanut oil, and palm oil as base oils. A K-P36 numerical-control precision surface grinder was used to perform plain grinding on a workpiece material with a high-temperature nickel base alloy. A YDM–III 99 three-dimensional dynamometer was used to measure grinding force,and a clip-type thermocouple was used to determine grinding temperature. The grinding force, grinding temperature, and energy ratio coefficient of MQL grinding were compared among the seven vegetable oil types. Results revealed that(1) castor oil-based MQL grinding yields the lowest grinding force but exhibits the highest grinding temperature and energy ratio coefficient;(2) palm oil-based MQL grinding generates the second lowest grinding force but shows the lowest grinding temperature and energy ratio coefficient;(3) MQL grinding based on the five other vegetable oils produces similar grinding forces, grinding temperatures, and energy ratio coefficients, with values ranging between those of castor oil and palm oil;(4) viscosity significantly influences grinding force and grinding temperature to a greater extent than fatty acid varieties and contents in vegetable oils;(5) although more viscous vegetable oil exhibits greater lubrication and significantly lower grinding force than less viscous vegetable oil, high viscosity reduces the heat exchange capability of vegetable oil and thus yields a high grinding temperature;(6) saturated fatty acid is a more efficient lubricant than unsaturated fatty acid; and(7) a short carbon chain transfers heat more effectively than a long carbon chain. Palm oil is the optimum base oil of MQL grinding, and this base oil yields 26.98 N tangential grinding force,87.10 N normal grinding force, 119.6 °C grinding temperature, and 42.7% energy ratio coefficient.     

卫星结构板涂装无机热控涂层工艺

对卫星结构板涂装无机白漆热控涂层工艺进行研究,考察了涂装前打磨工艺对结构板强度、涂层结合力的影响,并研究了较低温烘烤固化对涂装后无机白漆涂层外观、厚度、热辐射性能等的影响。结果表明:采用80#砂纸纵横交错打磨2～3遍能够满足无机涂层在结构板表面的附着力,且对0. 3 mm厚蒙皮结构板强度无影响,强度指标仍满足薄壁蜂窝夹层强度的要求。采用85℃/12 h的较低温烘烤工艺能够满足涂层外观、厚度、热辐射性能等各项指标要求。     

Specific grinding energy and surface roughness of nanoparticle jet minimum quantity lubrication in grinding

Nanoparticles with the anti-wear and friction reducing features were applied as cooling lubricant in the grinding fluid. Dry grinding, flood grinding, minimal quantity of lubrication（MQL）, and nanoparticle jet MQL were used in the grinding experiments. The specific grinding energy of dry grinding, flood grinding and MQL were 84, 29.8, 45.5 J/mm³, respectively. The specific grinding energy significantly decreased to 32.7 J/mm³ in nanoparticle MQL. Compared with dry grinding, the surface roughness values of flood grinding, MQL, and nanoparticle jet MQL were significantly reduced with the surface topography profile values reduced by 11%, 2.5%, and 10%,respectively, and the ten point height of microcosmic unflatness values reduced by 1.5%, 0.5%,and 1.3%, respectively. These results verified the satisfactory lubrication effects of nanoparticle MQL. MoS₂, carbon nanotube（CNT）, and ZrO₂ nanoparticles were also added in the grinding fluid of nanoparticle jet MQL to analyze their grinding surface lubrication effects. The specific grinding energy of MoS₂ nanoparticle was only 32.7 J/mm³, which was 8.22% and 10.39% lower than those of the other two nanoparticles. Moreover, the surface roughness of workpiece was also smaller with MoS₂ nanoparticle, which indicated its remarkable lubrication effects. Furthermore,the role of MoS₂ particles in the grinding surface lubrication at different nanoparticle volume concentrations was analyzed. MoS₂ volume concentrations of 1%, 2%, and 3% were used.Experimental results revealed that the specific grinding energy and the workpiece surface roughness initially increased and then decreased as MoS₂ nanoparticle volume concentration increased.Satisfactory grinding surface lubrication effects were obtained with 2% MoS₂ nanoparticle volume concentration.     

某航机燃烧室煤油改柴油燃烧特性研究

为了给某型航空发动机改为地面用柴油型燃气轮机的设计提供重要的技术支持,本文借助数值计算的方法,采用FLUENT稳态压力求解器、P1辐射模型和涡耗散破碎(EDU)燃烧模型对某航空发动机燃烧室在巡航工况和最大工况下煤油与柴油两种燃料的燃烧特性进行了计算及对比研究。得到了该燃烧室使用航空煤油(RP-3)和0号柴油的热态流场、空气流量分配、温度场、出口温度分布、污染物排放及头部燃油蒸发量。研究结果表明：当该燃烧室的燃料由航空煤油改为0号柴油后,燃烧室的热态温度场分布基本一致,流量分配最大差异在0.45%之内;燃烧效率降低约4.3%和NO、Soot排放量相当;出口温度分布和总压损失差异分别在1%和4.1%之内。     

Orbital phase spectroscopy of four high mass X-ray binary pulsars to study the stellar wind of the companion

Our work focuses on a comprehensive orbital phase-dependent spectroscopy of the four High Mass X-ray Binary Pulsars (HMXBPs) 4U 1538-52, GX 301-2, OAO 1657-415 and Vela X-1. We hereby report the measurements of the variation of the absorption column density and iron-line flux along with other spectral parameters over the binary orbit for the above-mentioned HMXBPs in elliptical orbits, as observed with the Rossi X-ray Timing Explorer (RXTE) and the BeppoSAX satellites. A spherically symmetric wind profile was used as a model to compare the observed column density variations. Out of the four pulsars, only in 4U 1538-52, we find the model having a reasonable corroboration with the observations, whereas in the remaining three the stellar wind seems to be clumpy and a smooth symmetric stellar wind model appears to be quite inadequate in explaining the data. Moreover, in GX 301-2, neither the presence of a disk nor a gas stream from the companion was validated. Furthermore, the spectral results obtained in the case of OAO 1657-415 and Vela X-1 were more or less similar to that of GX 301-2.     

焊后热处理对高温运行10CrMo910钢管接头持久寿命的影响

本文通过１０ＣｒＭｏ９１０钢大口径厚壁管道高温模拟试验证实，焊后热处理是一个短时超高温运行过程，它使１０ＣｒＭｏ９１０钢管接头组织提前老化，显著降低了接头的持久寿命。试验结果表明，传统的焊后热处理工序应当取消。     

航空精密工件高精磨削的研究

零件在外圆磨床上加工时受两个力的作用,一是受零件磨削力的影响,二是受外圆磨床尾座对顶力的影响,尤其细长杆零件受力变形较为明显。为了在加工过程中避免零件变形而影响加工精度,通过使用ANSYS对零件进行有限元分析,控制两个方向力的大小,并对这两个方向力进行逐一分析,并配合高速磨削加工,确定进刀量、磨削速度、零件转速及对顶力等磨削参数,并对上述分析方法进行延伸扩展。     

The Crab pulsar seen with AquEYE at Asiago Cima Ekar observatory

We are developing fast photon-counter instruments to study the rapid variability of astrophysical sources by time tagging photon arrival times with unprecedented accuracy, making use of a Rubidium clock and GPS receiver. The first realization of such optical photon-counters, dubbed AquEYE (the Asiago Quantum Eye), was mounted in 2008 at the 182 cm Copernicus Observatory in Asiago. AquEYE observed the Crab pulsar several times and collected data of extraordinary quality that allowed us to perform accurate optical timing of the Crab pulsar and to study the pulse shape stability on a timescale from days to years with an excellent definition. Our results reinforce the evidence for decadal stability of the inclination angle between the spin and magnetic axis of the Crab pulsar. Future realizations of our instrument will make use of the Galileo Global Navigation Satellite System (GNSS) time signal.     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.