A Statistical Study of the Mass Distribution of Neutron Stars

By reviewing the methods of mass measurements of neutron stars in four different kinds of systems, i.e., the high-mass X-ray binaries (HMXBs), low-mass X-ray binaries (LMXBs), double neutron star systems (DNSs) and neutron star-white dwarf (NS-WD) binary systems, we have collected the orbital parameters of 40 systems. By using the boot-strap method and the Monte-Carlo method, we have rebuilt the likelihood probability curves of the measured masses of 46 neutron stars. The statistical analysis of the simulation results shows that the masses of neutron stars in the X-ray neutron star systems and those in the radio pulsar systems exhibit different distributions. Besides, the Bayes statistics of these four different kind systems yields the most-probable probability density distributions of these four kind systems to be (1.340 ± 0.230)M8, (1, 505 ± 0.125)M8,(1.335 ± 0.055)M8 and (1.495 ± 0.225)M8, respectively. It is noteworthy that the masses of neutron stars in the HMXB and DNS systems are smaller than those in the other two kind systems by approximately 0.16M8. This result is consistent with the theoretical model of the pulsar to be accelerated to the millisecond order of magnitude via accretion of approximately 0.2M8. If the HMXBs and LMXBs are respectively taken to be the precursors of the BNS and NS-WD systems, then the influence of the accretion effect on the masses of neutron stars in the HMXB systems should be exceedingly small. Their mass distributions should be very close to the initial one during the formation of neutron stars. As for the LMXB and NS-WD systems, they should have already under- gone the process of suffcient accretion, hence there arises rather large deviation from the initial mass distribution.     

A Statistical Study of the Relation between the Amplitude of Solar Cycle and the Area of Active Regions

Based on the observational data of sunspots, the relation between the amplitude of solar cycle and the total area of all active regions occurred in a solar cycle has been investigated. The result shows that the amplitude of solar cycle has a good correlation with the total area of all active regions occurred in the solar cycle. The relation between the amplitude of solar cycle and the area of the largest active region during a solar cycle has also been investigated. The result shows that the amplitude of solar cycle has a poor correlation with the area of the largest active region during a solar cycle, and there is no fixed relation between the peak time of a solar cycle and the time when the largest active region occurred in the solar cycle.     

The environmental dependence of different colors in the CMASS sample of the SDSS DR9

I investigate the environmental dependence of galaxy colors in the CMASS sample of the Sloan Digital Sky Survey Data Release 9(SDSS DR9).To decrease the radial selection effect,I divide the CMASS sample into subsamples with a redshift binning size of?z=0.01 and analyze the environmental dependence of the u-r,u-g,g-r,r-i and i-z colors for these subsamples in each redshift bin.Statistical analysis shows that all five colors weakly correlate with the local environment,which may mean that the environmental processes responsible for a galaxy’s properties proceed slowly over cosmic time.     

Statistics of underwater ambient noise at high sea states arisen from typhoon out zones in the Philippine Sea and South China Sea

Oceanic noise is the background interference in sonar performance prediction and evaluation at high sea states. Statistics of underwater ambient noise during Typhoons Soulik and Nida were analyzed on the basis of experimental measurements conducted in a deep area of the Philippine Sea and the South China Sea. Generated linear regression, frequency correlation matrix (FCM), Burr distribution and Gumbel distribution were described for the analysis of correlation with environmental parameters including wind speed (WS), significant wave height (SWH), and the inter-frequency relationship and probability density function of noise levels (NLs). When the typhoons were quite close to the receivers, the increment of NLs exceeded 10 dB. Whilst ambient noise was completely dominated by wind agitation, NLs were proportional to the cubic and quintic functions of WS and SWH, respectively. The fitted results between NLs and oceanic parameters were different for “before typhoon” and “after typhoon”. The fitted slopes of linear regression showed a linear relationship with the logarithm of frequency. The average observed typhoon-generated NLs were 5 dB lower than the Wenz curve at the same wind force due to the insufficiently developed sea state or the delay between NLs and WS. The cross-correlation coefficient of FCM, which can be utilized in the identification of noise sources in different bands, exceeded 0.8 at frequencies higher than 250 Hz. Furthermore, standard deviation increased with frequency. The kurtosis was equal to 3 at >400 Hz approximately. The characteristics of NLs showed good agreement with the results of FCM.     

基于空间计量模型的城市网络外部性定量测度

在经济全球化、区域一体化的背景下,城市发展动力由内部功能集聚转向外部关系协调,城市间的关联作用愈发重要,成为“城市的第二本质”。通过文献计量分析,发现空间计量模型逐渐成为城市网络外部性定量测度的主要方法之一。从研究设计角度,空间计量模型作为城市网络外部性的定量建模工具,存在至少两方面的问题：城市网络外部性的非对称效应和城市网络的多尺度问题。本文结合城市网络外部性测度与建模,首先阐述如何规范地解读空间计量模型参数及其与网络外部性测度的对应关系;其次基于蒙特卡洛模拟实验论证非对称城市网络外部性和多尺度城市网络外部性的建模方法。研究表明：(1)忽视城市网络外部性中潜在的非对称效应会显著降低模型参数估计的准确性,本文开发的非对称空间效应模型（Asymmetric Spatial Econometric Model,ASEM）可以准确识别网络外部性的非对称效应,给出更加准确的参数估计;(2)忽略现实存在的多尺度网络效应,只在单一尺度对网络效应建模会造成参数估计失真,而空间多尺度统计模型（Hierarchical Spatial Autoregressive model,HSAR）为多尺度网络外部...     

A SCUBA scan-map of the Hubble Deep Field: measuring the bright end of the submillimetre source counts

Using the 850-μm SCUBA camera on the JCMT and a scanning technique different from other sub-mm surveys, we have obtained a 125 arcmin² map centred on the Hubble Deep Field . The 1 σ sensitivity to point sources is roughly 3 mJy and thus our map probes the brighter end of the sub-mm source counts. We find six sources with a flux greater than about 12 mJy (>4 σ ) and, after a careful accounting of incompleteness and flux bias, estimate the integrated density of bright sources     (68 per cent confidence bounds).