|
|
|
题名
|
作者
|
年代
|
出处
|
被引量
|
| 1 | 乌鲁木齐天文站25m天线18cm脉冲星脉冲到达时间观测系统显示文摘脉冲星脉冲到达时间观测系统建立在25m射电天线的18cm波段上,消色散采用了2x128x2.5MHz多通过滤波器和数字化器,数据采集系统由PC机完成.1999年5月至6月间建立了基于常温接收机的到达时间观测系统.观测到的最弱源的平均流量密度为4mJy. | 张晋 张晋 吴鑫基 吴鑫基 王娜 王娜 王娜 王娜 艾力.玉 艾力.玉 K.S.Cheng | 1999 | 天体物理学报1999，19，4： | 8 |
| 2 | Gamma-Ray Bursts: Afterglows and Central Engines显示文摘Gamma-ray bursts (GRBs) are the most intense transient gamma-ray events in the sky; this, together with the strong evidence (the isotropic and inhomogeneous distribution of GRBs detected by BASTE) that they are located at cosmological distances, makes them the most energetic events ever known. For example, the observed radiation energies of some GRBs are equivalent to the total convertion into radiation of the mass energy of more than one solar mass. This is thousand times stronger than the energy of a supernova explosion. Some unconventional energy mechanism and extremely high conversion efficiency for these mysterious events are required. The discovery of host galaxies and association with supernovae at cosmological distances by the recently launched satellite of BeppoSAX and ground based radio and optical telescopes in GRB afterglow provides further support to the cosmological origin of GRBs and put strong constraints on their central engine. It is the aim of this article to review the possible central engines, energy mechanisms, dynamical and spectral evolution of GRBs, especially focusing on the afterglows in multi-wavebands. | K.S.Cheng T.Lu | 2001 | Chinese Journal of Astronomy and Astrophysics2001，1，1： | 8 |
| 3 | A Two-Temperature Supernova Fallback Disk Model for Anomalous X-ray Pulsars显示文摘We present a case study of the relevance of the radially pulsational instability of a two-temperature accretion disk around a neutron star to anomalous X-ray pulsars (AXPs). Our estimates are based on the approximation that such a neutron star disk with mass in the range of 10-6-10-5 M⊙ is formed by supernova fallback. We derive several peculiar properties of the accretion disk instability: a narrow interval of X-ray pulse periods; lower X-ray luminosities; a period derivative and an evolution time scale. All these results are in good agreement with the observations of the AXPs. | YeLu K.S.Cheng | 2002 | Chinese Journal of Astronomy and Astrophysics2002，2，2： | 0 |
| 4 | On the Light Curve and Spectra of X-Rays and Gamma-Rays from the Crab Pulsar显示文摘We use a three-dimensional pulsar magnetosphere model to study the light curve and spectra of x-rays and gamma-rays from the Crab pulsar. In this model, the vertical size of the outer gap is first determined by a self-consistent model in which the outer gap is limited by pair production from collisions of thermal photons produced by polar cap heating of backflow outer gap current and curvature photons emitted by gap accelerated charged particles. The transverse size of the outer gap is determined by local pair production conditions. In principle, there are two topologically disconnected outer gaps present in the magnetosphere of a pulsar, and both incoming and outgoing particle flows are allowed. However, double-peak light curves with strong bridges are most common, Making use of the three-dimensional structure of the outer gap and its local properties, we compare the results of our model with the light curve and phase-resolved spectra of the Crab pulsar. | 张力 K.S.Cheng 梅冬成 | 2000 | Chinese Physics Letters2000，17，7： | 0 |
| 5 | Cosmic-Ray Positrons Produced by Pulsar Winds from Mature Gamma-Ray Pulsars显示文摘In the frame of theγ-ray pulsar outer gap model,e^(±)pairs in the pulsar magnetosphere are produced by the cascade of e^(±)pairs through synchrotron radiation of the return current from the outer gap.These pairs are accelerated mono-energetically to relativistic energies in the pulsar wind driven by low-frequency electromagnetic waves.Using Monte Carlo simulations,we generate a sample of the matureγ-ray pulsars in our Galaxy and calculate the positron production rate from these pulsars.With a simple leaky box model,we calculate the ratio of cosmic-ray positron to total electrons.Our result indicates that the pulsar contribution to the cosmic ray positron peaks at about 40 GeV and the observed e^(+)/(e^(-)+e^(+))ratio can be explained by this model. | 张力 K.S.Cheng 梅冬成 | 2001 | Chinese Physics Letters2001，18，5： | 0 |
您所在的机构暂未开通此部分的功能，请联系管理员