ALMA observations of the circumstellar envelope around EP Aqr

Atacama Large Millimetre/sub-millimetre Array(ALMA) observations of CO(1–0) and CO(2–1) emissions from the circumstellar envelope of the asymptotic giant branch(AGB) star EP Aqr have been made with four times better spatial resolution than previously available. They are analysed with emphasis on the de-projection in space of the effective emissivity and flux of matter using as input a prescribed configuration of the velocity field, assumed to be radial. The data are found to display an intrinsic axisymmetry with respect to an axis making a small angle with respect to the line of sight. A broad range of wind configurations, from prolate(bipolar) to oblate(equatorial) has been studied and found to be accompanied by significant equatorial emission. Qualitatively, the effective emissivity is enhanced near the equator to produce the central narrow component observed in the Doppler velocity spectra and its dependence on star latitude generally follows that of the wind velocity with the exception of an omni-present depression near the poles. In particular, large equatorial expansion velocities produce a flared disc or a ring of effective emissivity and mass loss. The effect on the determination of the orientation of the star axis of radial velocity gradients, and possibly competing rotation and expansion in the equatorial disc, is discussed. In general,the flux of matter is found to reach a broad maximum at distances of the order of 500 AU from the star.Arguments are given that may be used to favour one wind velocity distribution over another. As a result of the improved quality of the data, a deeper understanding of the constraints imposed on morphology and kinematics has been obtained.     

New photometric investigation of the low-mass-ratio contact binary star V1853 Orionis

Four-color charge-coupled device(CCD) light curves in the B, V, Rc and I c bands of the totaleclipsing binary system V1853 Orionis(V1853 Ori) are presented. By comparing our light curves with those published by previous investigators, it is determined that the O'Connell effect on the light curves has disappeared. By analyzing those multi-color light curves with the Wilson-Devinney code(W-D code),it is discovered that V1853 Ori is an A-type intermediate-contact binary with a degree of contact factor of f = 33.3%(3.7%) and a mass ratio of q = 0.1896(0.0013). Combining our 10 newly determined times of light minima together with others published in the literature, the period changes of the system are investigated. We found that the general trend of the observed minus calculated(O-C) curve shows a downward parabolic variation that corresponds to a long-term decrease in the orbital period with a rate of d P/dt =-1.96(0.46)×10^-7 d yr^-1. The long-term period decrease could be explained by mass transfer from the more-massive component to the less-massive one. By combining our photometric solutions with data from Gaia DR_2, absolute parameters were derived as M_1 = 1.20 M⊙, M_2 = 0.23 M⊙, R_1 = 1.36 R⊙and R_2 = 0.66 R⊙. The long-term period decrease and intermediate-contact configuration suggest that V1853 Ori will evolve into a high fill-out overcontact binary.     

The symmetry energy and incompressibility constrained by the observations of glitching pulsars

We investigate the masses of glitching pulsars in order to constrain their equation of state(EOS). The observations of glitches(sudden jumps in rotational frequency) may provide information on the interior physics of neutron stars. With the assumption that glitches are triggered by superfluid neutrons, the masses of glitching neutron stars can be estimated using observations of maximum glitches.Together with the observations of thermal emission from glitching pulsars Vela and J1709–4429, the slope of symmetry energy and incompressibility of nuclear matter at saturation density can be constrained.The slope of symmetry energy L should be larger than 67 MeV while the lower limit of incompressibility for symmetric nuclear matter K_0 is 215 MeV. We also obtain a relationship between L and K_0:6.173 MeV + 0.283 K_0≤ L ≤ 7.729 MeV + 0.291 K_0. The restricted EOSs are consistent with the observations of 2-solar-mass neutron stars and gravitational waves from a binary neutron star inspiral.     

移动扫描系统在1∶2 000地形图成果检验中的应用

基于移动扫描系统提出一套新的1∶2 000地形图检验流程,通过与全站仪、RTK等传统数学精度检验方式,论证移动扫描系统三维点云数学精度对于1∶2 000地形图精度检测的适用性。通过与传统人工外业巡视等传统地理精度检验方式,对比、分析全景影像对于地理精度检测的辅助作用。实验结果表明,移动扫描系统的三维点云数据数学精度符合1∶2 000地形图测绘成果质量精度检测要求,以全景影像辅助地理精度检查一定程度降低外业检验时长。因此,将移动扫描系统运用于1∶2 000等大比例尺地形图成果质量检验工作能一定程度优化检验流程、提升质检效率,为测绘成果质量检验工作提供新思路。     

1：500DLG数据的质量控制与质量评价

DLG数据是城市地形要素的主要表达形式,如何对DLG数据的采集过程进行质量控制、质量检查,如何对DLG数据进行客观的质量评价,是值得探讨和研究的问题。本文针对1：500DLG数据生产的各个环节,全面介绍了其质量控制、质量检查、质量验收、质量评定的内容和方法。     

1：100万图号中行号、列号正误的快速判断方法

针对多个县(市)、区土地调查文字材料将1:100万图号中的行、列号用错而产生严重缺陷的事实,本人认真学习了"国家基本比例尺地形图分幅和编号"的基础知识,并总结归纳出简易的快速判断正误的方法,以杜绝类似差错的发生.     

1:5万区域化探样品分析测试的质量监控

依据《地质矿产实验室测试质量管理规范》,并结合山西省的地质情况建立了一套1:5万区域化探样品分析测试的质量监控体系。分四个部分详细论述了的1:5万区域化探样品分析测试的质量监控体系。过去1:5万质量监控体系完全是靠人工进行,效率低下;本质量监控体系与过去相比,不但节省了大量的人力、物力,而且更加准确、迅速,更能适应1:5万质量监控大量数据处理的需要。     

日照市近岸夜光藻生消特征及其与水温和营养盐的关联

为摸清日照近岸夜光藻赤潮爆发规律,以有效防控夜光藻赤潮,本研究在日照市近岸海域选择3个监测站点,监测水文气象因子、化学因子和浮游植物。结果显示：日照市海区夜光藻赤潮爆发区多位于近海海区。夜光藻赤潮爆发时间在3—4月份,夜光藻密度南低北高。日照市海区夜光藻属冷水种,6℃开始爆发生长,18℃消亡。三月初夜光藻优势度在0.2～0.3之间,三月中旬到四月初夜光藻优势度逐渐增大,最大达0.99。夜光藻爆发时,无机氮0.2～0.3 mg/L。夜光藻爆发初期活性磷酸盐浓度高于末期,且随着夜光藻密度增加而升高。磷元素是夜光藻爆发的限制因子。夜光藻赤潮过程复杂,受物理、化学、生物、气象等多重因素的综合影响。日照市夜光藻具有冷水性特征。     

1:500航测综合法成图的探讨

本文扼要地叙述了1:500航测综合法成图的工艺流程及作业中应注意的问题,并以无锡市测区的成图精度,证实了该项工艺流程及作业方法的可行性。