Spectral hardening of cosmic ray protons and helium nuclei in supernova remnant shocks

The observed hardening of the spectra of cosmic ray protons and helium nuclei is studied within the model of nonlinear diffusive shock acceleration of supernova remnants(SNRs). In this model, the injected particles with energies below the spectral "knee" are assumed to be described by two populations with different spectral indexes around 200 GeV. The high-energy population is dominated by the particles with energies above 200 GeV released upstream of the shock of SNR, and the low-energy population is attributed to the particles with energies below 200 GeV released downstream of the shock of SNR. In this scenario, the spectral hardening of cosmic ray protons and helium nuclei observed by PAMELA, AMS-02, and CREAM experiments can be reproduced.     

Multiband Non-Thermal Radiation from the Crab Nebula and the Pulsar Wind Nebula in MSH 15-52

We study the multiband non-thermal emission from two pulsar wind nebulae （PWNe）, the Crab nebula and the PWN in MSH 15-52. Both of them have been recently detected by the Fermi large area telescope （LAT） and powered by central gamma-ray pulsars. Motivated by the Fermi LAT results, we use a simplified time-dependent injection model to study the non-thermal emission from radio to very high energy gamma-ray radiation from these two sources. In this model, the relativistic electrons are accelerated in pulsar magnetosphere and at pulsar wind termination shocks and can be described by a broken power law. Those high energy particles evolve with time and produce non-thermal emission through synchrotron radiation and inverse Compton scattering of soft photons. For Crab nebula, using the GeV emission from 100 MeV to 10 GeV given by Fermi LAT, we can constrain the maximum energy of the electrons and other parameters. The non-thermal emission can be well explained by this model. We also use this model to explain the non-thermal emission from the PWN in MSH 15-52.     

Fluxes and Death Lines of Gamma-Ray Pulsars

We study the fluxes and the death lines of γ-ray emission of the pulsars with outer gaps.In a self-sustained outer gap,we derive that the fractional size of the outer gap is a function of period,period derivative,radial distance and magnetic inclination angle for a pulsar.Our results indicate that (i) averaged typical γ-ray energy and γ-ray flux of a pulsar with an outer gap increase with the magnetic inclination angle;we estimate the averaged γ-ray fluxes for observed canonical pulsars with outer gaps and compare them with the sensitivities of AGILE and GLAST,and (ii) if the fractional size of the outer gap at the inner boundary of the outer gap is not greater than unity,then an outer gap exists;such a condition gives the death lines of the pulsars with outer gaps.     

采用简化燃烧室研究柴油机缸内流动

本文采用简化燃烧室研究柴油机燃烧室结构参数对涡流比的影响.简化燃烧室排除了实际燃烧室边界形状的复杂性,主要结构参数之间的可比性更强.研究表明,缸内总体平均涡流比遵循角动量守恒定律,由流体平均旋转半径、角动量、以及摩擦耗散决定.上止点附近,横截面上的平均涡流比除受上述三种因素影响外,还受燃烧室内涡环的影响,涡环的强弱取决于活塞凹坑形式;横截面切向速度分布因受涡环影响,而不能简单归结为刚体流与势流的组合.     

内燃机气道及缸内气体流动特性研究

本文对某型号内燃机气道稳态流动和缸内气流运动特性进行了研究.气道流动特性稳态计算结果与气道稳流试验结果相吻合,流动特征参数偏差在3%左右.瞬态计算结果表明,在进气行程初期,缸内涡流和湍流迅速增强,随后涡流变化缓慢,而湍流强度迅速下降.在气门叠开时,存在进气和排气回流现象.进气时,进气阀边缘处是缸内气体最大速度出现位置,气门最大升程时该处速度达到134.4m/s;切向气道缩口处最大速度高达134.7m/s,此处存在一定的进气节流损失.     

Effect of Gamma-Ray Beaming on the Fluxes of Gamma-Ray Pulsars

We study the effect of γ-ray beaming on γ-ray emission of the pulsars in a self-sustained outer gap model. In this model, averaged γ-rav flux is a function of period, magnetic field, magnetic inclination angle and solid angle of γ-ray beaming for a γ-ray pulsar. We generate a sample of γ-ray pulsars with their ages less than 10^6 ears by using the Monte Carlo method, and then study the γ-ray beaming effect. The comparison of distributions of periods, magnetic fields, distances, γ-ray energy fluxes and period derivatives of the simulated γ-ray pulsars with those of observed γ-ray pulsars by the detector EGRET shows that γ-ray beaming has an important role on the detection of γ-ray pulsars. Furthermore, possible γ-ray pulsars observed by the detector GLAST are predicted.