蟹状星云脉冲星的TeV γ射线周期发射

利用自行研制的两台大气切伦科夫望远镜(ACT2和ACT3),在1995年秋至1996年春的观测季节对蟹状星云脉冲星进行了168小时(ACT2)和126小时(ACT3)的跟踪观测.分析这些数据没有发现有月或天时间尺度稳定的33ms周期的TeVγ射线发射,但发现两段持续几十分钟的暴发样本具有33ms周期.     

Central black hole masses of galaxies

In this paper, the stellar velocity dispersions in the host galaxies are used to estimate the central black hole masses for a sample of elliptical galaxies. We find that the central black hole masses are in the range of 10^{(5.5-9.5)}M_⊙. Based on the estimated masses in this paper and those by Woo & Urry (2002) and the measured host galaxy absolute magnitude, a relation, log (M_{BH}/M_⊙) = -(0.25±4.3×10^{-3})M_R + (2.98±0.208) is found for central black hole mass and the host galaxy magnitude. Some discussions are presented.     

An X-ray luminosity analysis for FRIs and FRIIs

Radio galaxies are divided into two groups according to their luminosities at 178 MHz, namely Fanaroff-Riley type Is (FRIs) and Fanaroff-Riley type IIs (FRIIs) with FRIs showing lower radio luminosities than FRIIs. In this paper, the X-ray data are compiled for 183 radio galaxies (61 FRIs and 122 FRIIs), from the available literature, for the analysis of the X-ray properties. The 1 keV X-ray luminosities are calculated and discussed for the two groups, and an averaged X-ray luminosity of logL _X^{1 keV} = 41.30±2.51 erg·s⁻¹·keV⁻¹ is found for FRIs, which is lower than that for FRIIs, logL _X^{1 keV} = 43.39±3.06 erg·s⁻¹·keV⁻¹. A Kolmogorov-Smirnov (K-S) test indicates that the probability for the X-ray luminosity distributions of the two groups to be from the same parent distribution is 1.44×10⁻¹⁰. We also discuss the origin and the mechanism of the X-ray emission for FRIs and FRIIs. Supported by the National Natural Science Foundation of China (Grant Nos. 10573005 and 10633010) and the National Basic Research Program of China (Grant No. 2007CB815405)     

Statistical properties of extragalactic radio sources

In this paper, a large sample of extragalactic radio sources is analysed to show their statistical properties. The core and total radio powers are used to determine the core-dominance parameter for galaxies, BL Lacertae objects and quasars; mutual correlations between core radio power, total radio power, redshift and core dominance parameter are examined for different subclasses. A statistically significant correlation between the total and core radio power is confirmed. There are no obvious correlations between core-dominance parameter and the total power for our whole sample and quasars, but there is a statistically significant anti-correlation for our galaxy sample. Some discussions and comparison of the correlations with those obtained by other authors are also given.     

A comparison between repeating bursts of FRB 121102 and giant pulses from Crab pulsar and its applications

There are some similarities between bursts of repeating fast radio bursts (FRBs) and giant pulses (GPs) of pulsars. To explore possible relations between them, we study the cumulative energy distributions of these two phenomena using the observations of repeating FRB 121102 and the GPs of Crab pulsar. We find that the power-law slope of GPs (with fluence≥130 Jy·ms) is 2.85±0.10. The energy distribution of FRB 121102 can be well fitted by a smooth broken power-law function. For the bursts of FRB 121102 above the break energy (1.22 ×10³⁷ erg), the best-fitting slope is {2.90}_{-0.44}^{+0.55}, similar to the index of GPs at the same observing frequency (∼1.4 GHz). We further discuss the physical origin of the repeating FRB 121102 in the framework of the super GPs model. And we find that the super GPs model involving a millisecond pulsar is workable and favored for explaining FRB 121102 despite that the magnetar burst model is more popular.     

Mössbauer search for the DX-center

Hyperfine Interactions - A survey is given of a number of Mössbauer studies on Te in GaAs and AlxGa1−xAs. It is discussed what can be learned from these studies on the socalled...     

The Mössbauer search for Fe in Si

In this review paper, a series of Mössbauer experiments on Fe in Si, spread over almost thirty years, is discussed. In early Mössbauer experiments, the role of precipitate formation during diffusion was insufficiently realized. Later, an apparent inconsistency was observed between ion implantation experiments by recoil implantation of Coulomb excited atoms and by conventional ion implantation. This inconsistency is removed by recent high-resolution Coulomb excitation recoil implantation studies and by ion implantation experiments at the temperature of liquid helium. These studies lead to an unambiguous identification of interstitial Fe and Co in Si. Finally, the present status of the theoretical predictions on the isomer shift of Fe in Si is reviewed.     

Extracting Energy Magnetically from Plunging Region of Black-Hole Accretion Disk

An analytical expression for the jet power extracted from the plunging region between a black hole (BH)horizon and the inner edge of the disk (hereafter the PL power) is derived based on an improved equivalent circuit in BH magnetosphere with a mapping relation between the radial coordinate of the plunging region and that of the remote astrophysical load.It is shown that the PL power is of great importance in explaining jet power and dominates over the BZ and DL powers for a wide value range of the BH spin.In addition,we show that the PL power derived in our model can be fitted with the strong jet powers of several 3CR FR I radio galaxies,which cannot be explained by virtue of the BZ mechanism.Furthermore,the condition for negative energy of the accreting particles in the plunging region is discussed with the validity of the second law of BH thermodynamics.     

脉冲星自主天文导航概述

脉冲星因其具有良好的周期性,成为了非常良好的天文导航信号源,经过多年的观测分析,大量脉冲星的基本观测量已经被精确测定,通过理论模型分析,脉冲到达时间可以作为导航滤波的基本观测量,能提供时间与空间位置信息,因此,脉冲星可以为近地轨道和深空探测提供导航信息,从而替代传统的GPS导航定位以及深空网导航。介绍了脉冲导航的发展历程、脉冲星导航基本原理以及脉冲星导航系统实现框架与应用,并对脉冲星导航系统的进一步发展的难点进行有效分析。     

Largest Terrestrial Electromagnetic Pulsar

The power spectrum formula of the synchrotron radiation generated by the electron and positron moving at the opposite angular velocities in homogenous magnetic field is derived in the Schwinger version of quantum field theory. It is surprising that the spectrum depends periodically on radiation frequency which means that the system composed from electron, positron, and magnetic field forms the pulsar.     

Faint Young Sun,Planetary Paleoclimates and Varying Fundamental Constants

The effect of a cosmic time variation of the gravitational constant on the solar luminosity evolution is studied. It is demonstrated that a varying gravitational constant can substantially affect the solar flux at the planetary orbits on geological time scales. Mean surface temperatures well above the freezing point of water can be achieved in this way throughout the Archean and Hadean, without invoking an increased greenhouse effect or a lower albedo. Instead of a monotonous decline of the solar flux in look-back time, due to a dim early Sun, we infer a flux minimum during the Early Proterozoic and Late Archean. In this epoch, the solar flux is capable of generating mean surface temperatures between 7^∘C and 12^∘C, as compared to the present 15^∘C. The flux then steadily increases, culminating in temperatures between 12^∘C and 19^∘C some 4.5 Gry ago, depending on the parameters chosen for the ‘standard’ Sun. This explains the absence of polar caps, and even warm oceans in the Archean and Hadean are possible at these temperatures. No change of the present 33 K greenhouse effect is required. As for Mars, we show that the solar flux at the Martian orbit before 3.8 Gyr was at least 90% of the present-day flux, so that mean surface temperatures above the freezing point could have been generated by CO₂ greenhouse warming. The time variation of the gravitational constant is such that the moderate dimensionless ratio ħ² H₀/(k₀ cm_π³) stays constant in cosmic time. There are stringent bounds on the logarithmic time derivative of the gravitational constant from lunar laser ranging and helioseismology, which indicate that the first-order derivative at the present epoch is too small to noticeably affect the solar luminosity evolution within the age of the Earth. However, higher-order derivatives have to be taken into account, as they do affect the solar flux in geologic look-back time. We consider the impact of a varying gravitational constant on the redshift scaling of the linear size of radio galaxies. The observed scaling exponent also enters the solar luminosity evolution. The age of the universe has a substantial imprint on planetary paleoclimates.     

Vacuum Outer-Gap Structure in Pulsar Outer Magnetospheres

We study the vacuum outer-gap structure in the outer magnetosphere of rotation-powered pulsars by considering the limit of trans-field height through a pair production process. In this case, the trans-field height is limited by the photon-photon pair production process and the outer boundary of the outer gap can be extended outside the light cylinder. By solving self-consistently the Poisson equation for electrical potential and the Boltzmann equations of electrons/positrons and γ-rays in a vacuum outer gap for the parameters of Vela pulsar, we obtain an approximate geometry of the outer gap, i.e. the trans-field height is limited by the pair-production process and increases with the radial distance to the star and the width of the outer gap starts at the inner boundary （near the null charge surface） and ends at the outer boundary which locates inside or outside the light cylinder depending on the inclination angle.     

无线电引信双源辐照效应研究

为了探索复杂电磁环境对无线电引信的作用规律,提出双辐射源电磁环境构建方法和试验方法,试验研究了无线电引信的双辐射源电磁环境效应,找到了使无线电引信意外起爆的双辐射源辐照频率组合方式和敏感阈值。发现双辐射源使无线电引信意外起爆的作用机理：引信天线及弹体接收到差频为多普勒频率的复合连续波信号,经自差机振荡器混频、检波管检波并滤波后,输出信号幅度较大的正弦波信号,经低频电路放大、信号整流积分及抗干扰惯性支路的共同作用,通过增幅速率选择电路,触发执行级电路误动作导致引信意外起爆。     

无线电引信双源辐照效应研究

为了探索复杂电磁环境对无线电引信的作用规律,提出双辐射源电磁环境构建方法和试验方法,试验研究了无线电引信的双辐射源电磁环境效应,找到了使无线电引信意外起爆的双辐射源辐照频率组合方式和敏感阈值。发现双辐射源使无线电引信意外起爆的作用机理:引信天线及弹体接收到差频为多普勒频率的复合连续波信号,经自差机振荡器混频、检波管检波并滤波后,输出信号幅度较大的正弦波信号,经低频电路放大、信号整流积分及抗干扰惯性支路的共同作用,通过增幅速率选择电路,触发执行级电路误动作导致引信意外起爆。     

Constraining fast radio burst progenitors with gravitational lensing

Fast Radio Bursts(FRBs)are new transient radio sources discovered recently.Because of the angular resolution restriction in radio surveys,no optical counter part has been identified yet so it is hard to determine the progenitor of FRBs.In this paper we propose to use radio lensing survey to constrain FRB progenitors.We show that,different types of progenitors lead to different probabilities for a FRB to be gravitationally lensed by dark matter halos in foreground galaxies,since different type progenitors result in different redshift distributions of FRBs.For example,the redshift distribution of FRBs arising from double stars shifts toward lower redshift than of the FRBs arising from single stars,because double stars and single stars have different evolution timescales.With detailed calculations,we predict that the FRB sample size for producing one lensing event varies significantly for different FRB progenitor models.We argue that this fact can be used to distinguish different FRB models and also discuss the practical possibility of using lensing observation in radio surveys to constrain FRB progenitors.     

基于S变换的脉冲星辐射脉冲信号检测

为了提高脉冲星辐射脉冲信号的检测速度和在低信噪比下的检测效果, 提出了一种基于S变换的脉冲星辐射脉冲信号检测算法. 文中证明了高斯白噪声S变换域功率谱服从自由度为2的卡方分布, 基于此对累积信号S变换域功率谱进行阈值处理,累加阈值处理后的时频功率谱作为统计量进行检测. 此外阈值处理后的功率谱也可用来测量脉冲星信号的时间延迟. 仿真实验验证了本文算法的有效性,其检测性能优于同类的基于高斯分布模型的检测算法, 同时还可以在一定精度下给出脉冲星信号的时间延迟值. 关键词： 脉冲星 卡方分布 S变换域检测 时延测量     

Status of the search for the Mössbauer effect in109Ag

Our search for the Mössbauer Effect in¹⁰⁹Ag using the self-absorption method is summarized. Measurements have been made using two different¹⁰⁹Cd-doped single-crystal silver samples. In our method the silver K_α and K_δ x rays, as well as, the 88-keV γ rays are considered. The results are analyzed using the ratio of the number of x-ray to γ-ray counts. A positive effect is observed.     

Axion search in the monochromatic M1 transition of 65Cu

A search for axion emission in ⁶⁵Cu1 was performed using 6 NaI crystals. If the axion exists its ratio to γ decay must be several orders of magnitude below the present theoretical limits.