Sporadic emission of ultra high energy gamma rays from crab pulsar

In a further study of sporadic emission from pulsars we find evidence for short lived intense emission from the Crab pulsar.     

微通道流动转捩数值模拟

应用CFD计算软件ANSYS CFX对水力直径为0.4mm的矩形截面微尺度通道中的气体流动进行了数值模拟.采用了3种流动模型,即γ-Re_θt转捩模型、层流模型和剪切应力输运（SST）模型,并将模拟结果与实验结果进行了对比.模拟结果表明:层流模型及SST模型不具有预测转捩的能力;γ-Re_θt转捩模型捕捉到了临界雷诺数且摩擦因数相对误差在20%以下.在未达到临界雷诺数之前,通道后部已经出现局部湍流区,且局部湍流区随着雷诺数的增大而增大.壁面摩擦因数的最低点对应的流向位置与通道中前后湍流区的交结位置几乎一致.      

Relationships between energetic storm particle events and interplanetary shocks driven by full and partial halo coronal mass ejections

We have analysed energetic storm particle (ESP) events in 116 interplanetary (IP) shocks driven by front-side full and partial halo coronal mass ejections (CMEs) with speeds $>$400 km s^?1during the years 1996–2015. We investigated the occurrence and relationships of ESP events with several parameters describing the IP shocks, and the associated CMEs, type II radio bursts, and solar energetic particle (SEP) events. Most of the shocks (57 %) were associated with an ESP event at proton energies $>$1 MeV.The shock transit speeds from the Sun to 1 AU of the shocks associated with an ESP event were significantly greater than those of the shocks without an ESP event, and best distinguished these two groups of shocks from each other. The occurrence and maximum intensity of the ESP events also had the strongest dependence on the shock transit speed compared to the other parameters investigated. The correlation coefficient between ESP peak intensities and shock transit speeds was highest (0.73 $\pm$ 0.04) at 6.2 MeV. Weaker dependences were found on the shock speed at 1 AU, Alfvénic and magnetosonic Mach numbers, shock compression ratio, and CME speed. On average all these parameters were significantly different for shocks capable to accelerate ESPs compared to shocks not associated with ESPs, while the differences in the shock normal angle and in the width and longitude of the CMEs were insignificant.The CME-driven shocks producing energetic decametric–hectometric (DH) type II radio bursts and high-intensity SEP events proved to produce also more frequently ESP events with larger particle flux enhancements than other shocks. Together with the shock transit speed, the characteristics of solar DH type II radio bursts and SEP events play an important role in the occurrence and maximum intensity of ESP events at 1 AU.     

Optical search for gamma-ray bursts

The preliminary results from optical search for light pulses associated with gamma ray bursts by means of the Czechoslovak Fireball Network plate collection at the Ondřejov observatory are given. Optical monitoring represents more than 7700 hours, but no real optical counterpart was found. Problems associated with the optical search for gamma ray bursts are discussed.     

基于γ-Re_(θt)转捩模型的低雷诺数翼型数值分析

通过综合运用Michel转捩判据和γ-Re_(θt)转捩模型的方法实现对低雷诺数翼型的气动分析。首先通过Michel转捩判据和层流分离位置分别估算转捩动量厚度雷诺数,然后分别用Langtry和Tomac提出的经验关系式计算转捩动量厚度雷诺数和转捩区长度,通过UDF(User-Defined Functions)将不同组的3个经验关联值写入Fluent软件对E387翼型(雷诺数为3×10~5)进行数值分析,并与试验值进行了对比。结果表明:基于Michel转捩判据比基于层流分离更能准确预测转捩位置,基于层流分离预测的转捩位置过于靠前,但是2种方法的气动力计算结果与试验值都比较吻合,Langtry和Tomac的经验关系式计算结果之间差别不大,Tomac方法能够计算出分离泡,且与Selig油流试验吻合较好。     

基于Gamma-Theta模型的固定转捩数值模拟研究

采用γ-~Reθt转捩模型,对NACA0012翼型的固定转捩进行数值模拟,计算了不同雷诺数下刚好激发转捩又不引起过大局部压力扰动和附加阻力的最低粗糙带高度,说明了γ-~Reθt模型模拟固定转捩的能力。通过计算低雷诺数下固定转捩来模拟高雷诺数下自然转捩,计算结果表明固定转捩可以较好地模拟自然转捩。这两种计算结果对风洞试验都有重要的指导意义。     

Observing the Sun at 20–650 MHz at Thermopylae with Artemis

Fine structure of type IV radio solar bursts with a great variety and complexity often give much information in different ways and enable estimation of various coronal characteristics. In this work, we expose our new method for fine structure revealing and separation of two basic kinds of type IV fine structure, as fibers and pulsations. We also estimate frequency drift of fibers from dynamic spectra, clean from continuous background, with a prototype method using 2-D Fourier transform and we estimate periodicities of fibers as well as pulsations with continuous wavelet transform. Working with the last method we found periodicities close to 3 min umbral oscillations and 5 min global solar oscillations.     

Remnants of compact binary mergers

We investigate the long-term evolution and observability of remnants originating from the merger of compact binary systems and discuss the differences to supernova remnants. Compact binary mergers expel much smaller amounts of mass at much higher velocities, as compared to supernovae, which will affect the dynamical evolution of their remnants. The ejecta of mergers consist of very neutron rich nuclei. Some of these neutron rich nuclei will produce observational signatures in form of gamma ray lines during their decay. The composition of the ejecta might even give interesting constraints about the internal structure of the neutron star. We further discuss the possibility that merger remnants appear as recently discovered ‘dark accelerators’ which are extended TeV sources which lack emission in other bands.     

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.