WR 146 – observing the OB-type companion

We present new radio and optical observations of the colliding-wind system WR 146 aimed at understanding the nature of the companion to the Wolf–Rayet (WR) star and the collision of their winds. The radio observations reveal emission from three components: the WR stellar wind, the non-thermal wind–wind interaction region and, for the first time, the stellar wind of the OB companion. This provides the unique possibility of determining the mass-loss rate and terminal wind velocity ratios of the two winds, independent of distance. Respectively, these ratios are 0.20±0.06 and 0.56±0.17 for the OB-companion star relative to the WR star. A new optical spectrum indicates that the system is more luminous than had been believed previously. We deduce that the 'companion' cannot be a single, low-luminosity O8 star as suggested previously, but is either a high-luminosity O8 star, or possibly an O8+WC binary system.     

汶川MS8.0地震:龙门山断裂两侧地壳各向异性的初步研究

利用中国地震局地质研究所地震动力学国家重点实验室在川西地区布设的大规模密集流动宽频带地震台阵记录的远震P波波形数据,分别采用波形互相关和加权叠加方法研究了地壳各向异性。作为初步结果,得到了龙门山断裂两侧4个宽频带流动台站的接收函数莫霍面Ps转换震相快波方向和分裂时间延迟。结果表明:1)波形互相关方法总体上优于方位加权叠加方法,它不但可以给出快波方位,而且可以给出快慢波的时间延迟;方位加权叠加方法测量结果存在不确定性,其原因在于难以确定介质各向异性对称轴的方位;同时采用上述2种不同方法研究地壳各向异性参数有助于判断测量结果的可靠性;2)四川盆地内快波偏振方位基本一致,表明四川盆地地壳整体性较好,横向非均匀变形较弱;3)以汶川地震主震的震中区为界,松潘-甘孜地块北侧快波偏振方位与龙门山断裂近于平行,表明在四川盆地坚硬地壳的阻挡作用下,龙门山断裂附近松潘-甘孜地块北侧可能存在中下地壳软弱物质沿断层向NE方向的扩张变形,而其南侧处于正向挤压的状态。该结果有助于解释汶川MS8.0地震的单侧破裂过程及其余震发育的特征     

中国早期日食记录研究进展

中国古代系统的日食记录始自春秋。自汉以至清代,整齐而完备。此前的夏、商、西周三代,日食记录零散而模糊。历来研究者众而难得定论。近年来由于天文计算方法和历史年代学的进展,早期日食记录的研究也获得新的成就。     

Radio galaxies with a 'double-double morphology'– I. Analysis of the radio properties and evidence for interrupted activity in active galactic nuclei

We present four Mpc-sized radio galaxies which consist of a pair of double-lobed radio sources, aligned along the same axis, and with a coinciding radio core. We call these peculiar radio sources 'double-double' radio galaxies (DDRGs) and propose a general definition of such sources: a 'double-double' radio galaxy consists of a pair of double radio sources with a common centre. Furthermore, the two lobes of the inner radio source must have a clearly extended, edge-brightened radio morphology. Adopting this definition, we find several other candidate DDRGs in the literature. We find that in all sources the smaller (inner) pair of radio lobes is less luminous than the larger (outer) pair, and that the ratio of 1.4-GHz flux density of these two pairs appears to be anticorrelated with the projected linear size of the inner source. Also, the outer radio structures are large, exceeding 700 kpc. We discuss possible formation scenarios of the DDRGs, and we conclude that an interruption of the jet-forming central activity is the most likely mechanism. For one of our sources (B 1834+620) we have been able observationally to constrain the length of time of the interruption to a few Myr. We discuss several scenarios for the cause of the interruption, and suggest multiple encounters between interacting galaxies as a possibility. Finally, we discuss whether such interruptions help the formation of extremely large radio sources.     

天文大潮对南海北部浮游动物生物量的影响

基于2020年8月至11月在南海北部获取的声学多普勒流速剖面仪观测数据,利用后向散射强度数据估算得到相对体积散射强度并用其表征浮游动物生物量的相对大小,对相对体积散射强度的半月变化与具有半月周期的潮流动能进行相关性分析,进而分析天文大潮对声学估算的浮游动物生物量的影响。结果表明：半月周期的相对体积散射强度与潮流动能之间呈负相关关系,即天文大潮时,潮流动能较强,水体相对体积散射强度较低,浮游动物生物量则较小,天文小潮时则情况相反。初步推测其原因为：天文大潮时,强潮流一方面导致浮游动物生存环境恶化,使其生物量下降,另一方面也改变了浮游动物垂直迁移特性,浮游动物迁移到近海底处使其难以被观测。     

Infrared emission from 6.7-GHz methanol maser sources

Near-infrared photometry was performed on 56 southern 6.7-GHz methanol maser sources. A simple spherically symmetric model of the radiative transfer through a dust shell was developed and used to study the conditions in the dust cloud in which the masers are produced. The parameters investigated were the size of the cloud, the spectral type of the embedded star, the optical depth of the dust cloud and the dust density distribution. It was found that the infrared colours of the models have a complex dependence on the parameters and that no unique combination of parameter values explains the spectral energy distribution of any particular source. The model effectively reproduces the far-infrared ( IRAS ) colours but cannot simultaneously explain the near-infrared colours for any of the observed sources.     

大质量恒星形成区样本外向流的高灵敏度搜寻

对13个大质量恒星形成区样本进行了SiO(2-1)、CH_3OH(2-1)和C~(34)S(2-1)热线的观测.在9个分子云核中,3条热线同时被探测到.这9个SiO探测中,有3个是新探测到的且它们强度都相对较弱.所有探测到的谱线都有较明显的线翼,这可能是外向流出现的证据.SiO谱线的线宽最宽,这也更进一步表明SiO辐射可能是来自高速的外向流,即更靠近外向流的激发源.估算了各分子谱线的旋转温度,柱密度和相对元素丰度.结果表明SiO和CH_3OH元素丰度之间有较好的相关性,相关系数R=0.77,但是SiO和C~(34)S元素丰度之间却没有任何相关性.     

基于接收函数的华南及邻区地壳结构研究

利用华南地块及邻区2007～2012年609个地震台站记录的约900个5.7级以上远震事件,获得各台站的接收函数,通过分析接收函数的形态变化了解各台站下方的地壳结构特征,然后再利用H-κ叠加搜索技术获得各台站下方的地壳厚度和波速比.结果显示,研究区的地壳结构表现为从沿海向内陆逐渐复杂的变化,地壳厚度也表现出由沿海向内陆...     

射电天线指向改正模型中轴系误差的完全表达式

为了提高射电天线的目标跟踪精度,采用直接法推导了射电天线轴系误差对指向的影响,并给出轴系误差指向改正模型的完全表达式,明确了指向改正模型中各轴系参数的定义,传统分项以及球谐函数所推导的轴系误差项为该模型的简化形式.基于此,评估得出基本参数改正模型中,因忽略轴系误差高次谐项而引起的指向精度损失可能达到1′′量级,具体需结合轴系误差大小而定;同时明确了基本参数改正模型(如22项指向模型)中与轴系误差有关的部分高次谐项系数的物理意义.为高精度轴系误差指向改正模型的建立提供了理论依据.     

A simple tool for assessing the completeness in apparent magnitude of magnitude–redshift samples

A new tool is proposed for finding out the completeness limit in apparent magnitude of a magnitude–redshift sample. The technique, closely related to the statistical test proposed by Efron & Petrosian, presents a real improvement compared to standard completeness tests. Namely, no a priori assumptions are required concerning the redshift-space distribution of the sources. It means in particular that neither the clustering nor the evolution of the mean number density of the galaxies affects the result of the search.