Are Seyfert 2 Galaxies without Polarized Broad Emission Lines More Obscured？     

Xin-Wen Shu  Jun-Xian Wang  Peng Jiang 《中国天文和天体物理学报》2008,8(2):204-210

New XMM-Newton data of seven Seyfert 2 galaxies with optical spectropolarimet- ric observations are presented. An analysis of the 0.5 - 10 keV spectra shows that four Seyfert 2 galaxies with polarized broad lines (PBLs) are absorbed by NH < 1024 cm-2, while two of three Seyfert 2 galaxies without PBLs show evidence of Compton-thick obscuration, support- ing the conclusion that Seyfert 2 galaxies without PBLs are more obscured than those with PBLs. Adding the measured obscuration indicators (NH, T ratio, and Fe Kα line EW) of six luminous AGNs to our previous sample improves the significance level of the difference in absorption from 92.3% to 96.3% for NH, 99.1% to 99.4% for T ratio, and 95.3% to 97.4% for Fe Kα line EW. The present results support and enhance the suggestions that the absence of PBLs in Seyfert 2 galaxies can be explained by larger viewing angles of the line of sight to the putative dusty torus, which leads to the obscuration of the broad-line scattering screen, as expected in the unification model.  相似文献   

Clustering Property of Wolf-Rayet Galaxies in the SDSS     

Wei Zhang  Xu Kong  Fu-Zhen Cheng 《中国天文和天体物理学报》2008,8(2):211-218

We have analysed, for the first time, the clustering properties of Wolf-Rayet (W-R) galaxies, using a large sample of 846 W-R galaxies selected from the Data Release 4 (DR4) of the Sloan Digital Sky Survey (SDSS). We compute the cross-correlation function between W- R galaxies and a reference sample of galaxies drawn from the DR4. We compare the function to the results for control samples of non-W-R star-forming galaxies that are matched closely in redshift, luminosity, concentration, 4000-A break strength and specific star formation rate (SSFR). On scales larger than a few Mpc, W-R galaxies have almost the same clustering amplitude as the control samples, indicating that W-R galaxies and non-W-R control galax- ies populate dark matter haloes of similar masses. On scales between 0.1-1 h-1 Mpc, W-R galaxies are less clustered than the control samples, and the size of the difference depends on the SSFR. Based on both observational and theoretical considerations, we speculate that this negative bias can be interpreted by W-R galaxies residing preferentially at the centers of their dark matter haloes. We examine the distribution of W-R galaxies more closely using the SDSS galaxy group catalogue of Yang et al., and find that ～82% of our W-R galaxies are the central galaxies of groups, compared to ～74% for the corresponding control galaxies. We find that W-R galaxies are hosted, on average, by dark matter haloes of masses of 1012,3 M☉, compared to 1012,1 M? For centrally-located W-R galaxies and 1012,7 M☉ For satellite ones. We would like to point out that this finding, which provides a direct observational support to our conjecture, is really very crude due to the small number of W-R galaxies and the incom- pleteness of the group catalogue, and needs more work in future with larger samples.  相似文献   

Distribution of 56Ni Yields of Type Ia Supernovae and its Implication for Progenitors     

Bo Wang  Xiang-Cun Meng  Xiao-Feng Wang  Zhan-Wen Han 《中国天文和天体物理学报》2008,8(1):71-80

The amount of 56Ni produced in Type Ia supernova (SN Ia) explosion is probably the most important physical parameter underlying the observed correlation of SN Ia lumi-nosities with their light curves. Based on an empirical relation between the 56Ni mass and the light curve parameter △m15, we obtained rough estimates of the 56Ni mass for a large sample of nearby SNe Ia with the aim of exploring the diversity in SN Ia. We found that the derived 56Ni masses for different SNe Ia could vary by a factor of ten (e.g., MNi = 0.1 - 1.3 M⊙),which cannot be explained in terms of the standard Chandraseldaar-mass model (with a 56Ni mass production of 0.4 - 0.8 M⊙). Different explosion and/or progenitor models are clearly required for various SNe Ia, in particular, for those extremely nickel-poor and nickel-rich producers. The nickel-rich (with MNi 0.8 M⊙) SNe Ia are very luminous and may have massive progenitors exceeding the Chandrasekhar-mass limit since extra progenitor fuel is required to produce more 56Ni to power the light curve. This is also consistent with the find-ing that the intrinsically bright SNe Ia prefer to occur in stellar environments of young and massive stars. For example, 75% SNe Ia in spirals have △m15 < 1.2 while this ratio is only 18% in E/S0 galaxies. The nickel-poor SNe Ia (with MNi < 0.2 M⊙) may invoke the sub-Chandrasekhar model, as most of them were found in early-type E/S0 galaxies dominated by the older and low-mass stellar populations. This indicates that SNe Ia in spiral and E/S0 galaxies have progenitors of different properties.  相似文献   

An Approach of Tropospheric Correction for VLBI Phase-Referencing using GPS Data     

Bo Zhang  Xing-Wu Zheng  Jin-Ling Li  Ye Xu 《中国天文和天体物理学报》2008,8(1):127-132

The dominant source of error in VLBI phase-referencing is the troposphere at observing frequencies above 5 GHz. We compare the tropospheric zenith delays derived from VLBI and GPS data at VLBA stations collocated with GPS antennas. The systematic biases and standard deviations both are at the level of sub-centimeter. Based on this agreement, we suggest a new method of tropospheric correction in phase-referencing using combined VLBI and GPS data.  相似文献   

基于小波变换的脉冲星弱信号的去噪方法研究   总被引：1，自引：0，他引：1  

汪丽  柯熙政  倪广仁 《天文研究与技术》2008,5(1):49-54

利用小波变换去除噪声的基本原理和方法及消色散方法对毫秒脉冲星极弱信号进行了提取,并对噪声进行了最佳阈值选取实验研究,实现了脉冲星弱信号消色散积累后的检测和抑噪.并研究了软硬阈值估计子等不同阈值消噪技术,进而对PSR 0437-4715信号采用不同方法去噪后的结果进行了分析比较,认为在最大分解层数J=5时对脉冲星信号处理有普适意义.研究结果认为基于小波变换的消噪方法是一种提高信噪比、展示噪声和突变信号的优越方法.  相似文献   

Possible Contribution of Mature γ-ray Pulsars to Cosmic-ray Positrons     

Quan-Gui Gao  Ze-Jun Jiang  Li Zhang 《中国天文和天体物理学报》2008,8(1)

We restudy the possible contribution of mature gamma-ray pulsars to cosmic ray positrons based on the new version of outer gap model. In this model, the inclination angle and average properties of the outer gap are taken into account, and more mature pulsars can have the outer gap and emit high energy photons. Half of the primary particles in the outer gaps will flow back toward the star surface and emit synchrotron photons, which can produce electron/positron pairs by the cascade of pair production. Some of these pairs will escape from the light cylinder and be accelerated to relativistic energies in the pulsar wind driven by low-frequency electromagnetic waves. Using a Monte Carlo method, we obtain a sample of mature gamma-ray pulsars and then calculate the production of the positrons from these pulsars. The observed excess of cosmic positrons can be well explained by this model.  相似文献   

SPOT 5卫星遥感影像在土地利用数据库系统更新中的应用     

刘天光  曹培国  孔琴 《山东国土资源》2007,23(6):2007/5/16-2007/6/25

随着国民经济的快速发展，土地现状变更十分频繁，如何保持数据库系统的现势性成为国土资源管理部门的一项重要工作。该文介绍了利用卫星遥感数据对土地利用数据库变更的系统设计、实现方法及结果，说明了利用遥感卫星数据对数据库进行更新的优势。  相似文献   

新疆春夏洪灾受灾面积长期变化趋势及其对农作物的影响   总被引：1，自引：0，他引：1  

王秋香  吴彦  叶殿秀  李秦 《干旱区地理》2009,32(3)

选用新疆1950-2006年84个县2038条洪水灾害资料,以春夏3～8月洪灾受灾面积为研究对象,用最小二乘法与二阶主值函数分析各月受灾面积的长期变化趋势,非参数化秩统计量做趋势的显著性检验,计算累计距平值判定时间序列的拐点,以拐点前后的变差系数比较受灾面积振幅的变化,采用morlet小波分析其振荡周期发现,春季3～5月农作物苗期是融雪洪水多发季节,洪灾受灾面积占全年的37%,各月受灾面积均有长期增加的趋势.其中,春季洪灾高发期的5月增加趋势十分显著,平均每年增加2.01%,是春季农田防洪的重点时期.夏季6～8月各种农作物的旺盛生长期,是暴雨洪水的频繁发生期,受灾面积占全年的60%,夏季各月洪灾受灾面积均有长期增加的趋势,其中,洪灾高发期的6、7月增加趋势十分显著,7月平均每年增加2.13%,6月增加1.86%,因此6、7月是夏季农田防洪的重点时期.另外,洪灾高发期的5、6、7月存在12～15年、5～7年的振荡周期,以及2～3年的小扰动,各类周期振荡在拐点之前比较弱,之后振荡较强.其中,春季3、4、5月拐点在1984年,夏季6、7、8月拐点分别在1974.年、1986年和1988年.同样以拐点为界,之前是洪灾少发时期,之后即开始处于洪灾频发期气候背景上的年代际与年际尺度振荡,另外,拐点前后平均受灾面积相差很大,增幅在58%～164%之间.  相似文献   

兰州-西宁城镇密集区经济联系的空间分析   总被引：6，自引：1，他引：5  

张志斌  赵睿琪 《干旱区地理》2009,32(3)

在经济全球化和信息化的今天,城镇密集区已成为全球经济体系的重要节点区域.文章首先用定性判断和定量计算的方法对兰州-西宁城镇密集区空间范围进行界定,然后从城镇的中心职能强度、城镇间经济联系强度和城镇经济辐射的空间范围三方面,对密集区33个主要城镇的经济联系状况进行测算.主要结论有:城镇中心地位的高低与其人口规模、经济实力及社会经济发展整体水平相关;中小城镇竖向联系强,横向联系弱,城镇间经济联系表现出明显的地域临近性;城镇经济影响范围的大小与其中地位的高低相对应,经济影响区界线存在重叠现象.  相似文献   

基于Ts-EVI特征空间的春旱遥感监测——以河北省为例   总被引：2，自引：0，他引：2  

闫峰  王艳姣  武建军 《干旱区地理》2009,32(5)

春季干旱是影响我国农业生产的重要自然灾害。以河北省为研究区,采用Ts-EVI构建的特征空间,以温度植被干旱指数TVDI作为土壤水分估算因子对2005年4～5月的春旱发生与发展进行遥感监测,主要得出以下结论:(1)表层土壤相对湿度RSM_(10)与TVDI的相关性均通过了α=0.001水平的置信度的t检验而表现出显著相关性,基于Ts-EVI特征空间构建的TVDI可以较好地估算土壤表层水分状况。(2)TVDI与不同土壤深度RSM的相关性在不同时期存在一定的差异,4月上旬～4月中旬以10 cm深度处的相关性最高,20 cm处次之;4月下旬～5月下旬以20 cm土壤深度处的相关性最好,10 cm处次之。(3)在不统计云覆盖地区旱情的情况下,2005年4月上旬河北省春旱面积为15 014.4 km~2;4月中旬～5月下旬的春旱面积分别为43 350.4 km~2、13 889.3km~2、71 664.3 km~2、12 864.8 km~2和44381.5 km~2。  相似文献