火焰稳定器射流喷口形状对燃烧性能的影响

为了探讨层缘吹气式火焰稳定器的射流喷口形状对燃烧性能的影响，在来流50m/s，573K条件下，分别对连续长缝、不连续宽缝、均布圆孔三种不同喷口形状的火焰稳定器的燃烧性能进行了实验研究，对比了它们的贫熄特性、燃烧效率和流阻损失。研究发现，在实验条件范围内，连续长缝形喷口稳定器的燃烧性能较其他两种不连续喷口稳定器优越，具有较高的燃烧效率、较宽的贫熄边界和较小的流阻损失。     

Grid-Adaptive Computations of Magnetized Jets

We present grid-adaptive numerical simulations of magnetized plasma jets, modeled by means of the compressible magnetohydrodynamic equations. The Adaptive Mesh Refinement strategy makes it possible to investigate long-term jet dynamics where both large-scale and small-scale effects are at play. We extend recent findings for uniformly magnetized, periodic shear layers to planar and fully 3D extended jet segments. The jet lengths cover multiple, typically 10, axial wavelengths of the fastest growing Kelvin–Helmholtz (KH) like modes. The dominant linear MHD instabilities of the jet flows are quantified by means of MHD spectroscopic analysis. In cases characterized by sonic Mach numbers about unity and large plasma beta values, both single and double shear layers (planar jets) manifest self-organizing trends to large scales, e.g. by continuous pairing/merging between co-rotating vortices, simultaneously with the introduction of small-scale features by magnetic reconnection events. The vortices form as a result of KH unstable shear-flow layers, and their coalescence arises from the growth of subharmonic modes at multiple wavelengths of the fastest growing KH instability. In extended two-dimensional jet segments, we investigate how varying jet width alters this coalescence process occurring at both edges, e.g. by introducing Batchelor-like coupling between counter-rotating vortices formed at opposing weakly magnetized, close shear layers. Finally, periodic segments of supersonic magnetized jets are simulated in two- and three-dimensional cases, which are characterized by violent shock-dominated transients.     

幂律型流体雾化SPH方法数值分析

幂律型流体的雾化过程存在复杂的界面运动,用传统网格法很难精确追踪运动界面.为研究幂律型流体的雾化特性,运用SPH方法对典型的双股幂律型流体撞击雾化问题进行三维数值分析.根据文献实验,采用SPH方法模拟获得与实验条件相应的数值结果,对比后表明,二者雾化角相当吻合,数值结果还成功捕捉到液膜向液丝的破碎过程及网状的液丝分布状态,验证了方法的有效性.分析了射流速度和撞击角度对雾化角的影响,得到雾化角随着射流速度和撞击角度的增加而增大;对雾化后的速度场进行数值分析后表明,撞击点附近,惯性力的作用使速度场变化剧烈;在流体远离撞击点的过程中,粘性耗散作用使速度场趋于稳定,但速度大小小于初始撞击速度.     

Analytical exact solutions for unsteady collisionless plume flows in a vacuum

This paper presents a set of gaskinetic solutions to the problem of unsteady collisionless round plume development: startup and development to a steady flow; steady flow; and shutting down from a steady flow. This can find applications in studying similar transient plume flows from space propulsion devices. Different from many past studies, here we consider the general situation that the average exit gas speed can be larger than zero, and detailed geometry of the nozzle exit radius is included. A fundamental space–velocity–time relation is adopted in this study and it plays a crucial role to obtain the complete flowfield properties of density, velocity, pressure and temperature. This study reveals that there are some internal complementary relations on density and momentum among these three processes. The results involve complex integrations involving factors of time, geometry, and specific speed ratio. Several numerical simulations with the direct simulation Monte Carlo method validate these analytical exact results.     

Protostellar Winds and Chondritic Meteorites

We discuss the interaction between the magnetosphere of a young star and its surrounding accretion disk. We consider how an X-wind can be driven magnetocentrifugally from the inner edge of the disk where accreting gas is diverted onto stellar field lines either to flow onto the Sun or to be flung outwards with the wind. The X-wind satisfies many observational tests concerning optical jets, Herbig-Haro objects, and molecular outflows. Connections may exist between primitive solar system materials and X-winds. Chondrules and calcium-aluminum-rich inclusions (CAIs) experienced short melting events uncharacteristic of the asteroid belt where meteorites originate. The inner edge of the solar nebula has the shortest orbital timescale available to the system, a few days. Protosolar flares introduce another timescale, tens of minutes to hours. CAIs may form when solids are lifted from shaded portions of the disk close to the Sun and are exposed to its intense light for a day or so before they are flung by the X-wind to much larger distances. Chondrules were melted, perhaps many times, by flares at larger distances from the Sun before being launched and annealed, but not remelted, in the X-wind. Aerodynamic sorting explains the narrow range of sizes with which CAIs and chondrules are found in chondritic meteorites. Flare-generated cosmic-rays may induce spallation reactions that produce some of the short-lived radioactivities associated with primitive solar system rocks. This revised version was published online in June 2006 with corrections to the Cover Date.     

GMRT monitoring of Cyg X-1 and Cyg X-3

We present the results of low frequency radio observations of the X-ray binaries, Cygnus X-1 and Cygnus X-3, during different X-ray states. The low frequency observations were made for the first time for these sources at 0.61 and 1.28 GHz using the Giant Meter-wave Radio Telescope (GMRT) between 2003 and 2004. Both Cyg X-1 and Cyg X-3 are highly variable at low radio frequencies. We also compare our data with the observations at 15 GHz conducted by the Ryle telescope. Spectral turnover is seen for both the sources below 2 GHz. The data suggest that the change in the radio flux density in both the sources is correlated to the X-ray hardness ratio and follows a similar behavior pattern.     

Acoustic measurements of models of military style supersonic nozzle jets

Modern military aircraft jet engines are designed with variable-geometry nozzles to provide optimal thrust in different operating conditions, depending on the flight envelope. How- ever, acoustic measurements for such nozzles are scarce, due to the cost involved in making full- scale measurements and the lack of details about the exact geometries of these nozzles. Thus the present effort at Pennsylvania State University （PSU） in partnership with GE Aviation and the NASA Glenn Research Center is aiming to study and characterize the acoustic field produced by supersonic jets issuing from converging-diverging military style nozzles, and to identify and test promising noise reduction techniques. An equally important objective is to develop methodology for using data obtained from small- and moderate-scale experiments to reliably predict the full-scale engine noise. The experimental results presented show reasonable agreement between small-scale and medium-scale jets, as well as between heated jets and heat-simulated ones.     

两点射流间隔时间对爆震波起爆特性影响的数值研究

为快速、短距起爆爆震波,本文基于H2/Air 8组分19步反应简化机理,采用两点射流点火的方法数值研究了不同射流管高度差引起的射流间隔时间对H2/Air混合物起爆特性的影响规律。采用与CEA计算结果及实验结果对比的方法验证了数值模拟的可靠性。结果表明,射流间隔时间对两点射流起爆有明显影响。一定射流间隔时间内可以成功起爆,但第一射流的衰减过程随射流间隔时间的增加而变长,不利于起爆。射流管的高度差使得射流管出口形成射流强度梯度,对射流强度的影响较小。射流管高度差ΔH的增加会加大两个射流之间的强度差,从而削弱射流相互作用。射流之间的相互作用受火焰面和压力面的共同影响,热点的形成更依赖于射流压力的相互作用。     

Radiation from relativistic shocks in turbulent magnetic fields

Using our new 3-D relativistic particle-in-cell (PIC) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron–positron jet propagating in an unmagnetized ambient electron–positron plasma. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value as predicted by hydrodynamic shock compression. In the jet (reverse) shock behind the bow (forward) shock the strongest electromagnetic fields are generated. These fields may lead to time dependent afterglow emission. In order to calculate radiation from first principles that goes beyond the standard synchrotron model used in astrophysical objects we have used PIC simulations. Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We then used the technique to calculate emission from electrons in a small simulation system. From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability. A fully developed shock within a larger simulation system may generate a jitter/synchrotron spectrum.