密近双星候选体LAMOST J051402.68+172659.7光谱分析  

Spectroscopic Analysis of Compact Binary Candidate LAMOST J051402.68+172659.7

作　　者：王琦 杨海峰[2] 蔡江辉 WANG Qi;YANG Hai-feng;CAI Jiang-hui(School of Mathematics and Information Technology,Yuncheng University,Yuncheng 044000,China;School of Computer Science and Technology,Taiyuan University of Science and Technology,Taiyuan 030024,China;School of Computer Science and Technology,North University of China,Taiyuan 030051,China)

机构地区：[1]运城学院数学与信息技术学院,山西运城044000 [2]太原科技大学计算机科学与技术学院,山西太原030024 [3]中北大学计算机科学与技术学院,山西太原030051

出　　处：《光谱学与光谱分析》2025年第5期1416-1421,共6页Spectroscopy and Spectral Analysis

基　　金：国家自然科学基金项目(12473105,12473106);山西省区域合作专项(202204041101037,202204041101033)资助。

摘　　要：密近双星系统通常具有更快速的轨道运动和更频繁的光变效应,以及伴星的快速演化,这使得它们成为研究星际物理过程和恒星演化的重要天体。测光图像和光变曲线是识别与证认双星的最常用手段,而如果当前观测技术无法分辨双目标的亮度和位置差异时,光谱型也是区分伴星成分的重要方法之一。采用基于粗集与聚类投票机制的光谱双星分析方法,对其离群目标LAMOST J051402.68+172659.7的光谱特征及其证认进行了深入分析。首先,针对LAMOST DR10发布的光谱双星(类别为DoubleStar),对其多次聚类结果投票数最低的17个目标光谱,进行了人眼筛查,除了大部分光谱信噪比较低外,LAMOST J051402.68+172659.7的两次观测光谱呈现较大差异;对于该目标的两次观测,其光谱一次呈现F型,一次呈现F+M型,在排除邻近光纤污染和目标所处环境中其他目标污染后,确定两次观测光谱上呈现的都是目标真实成分,揭示了两种光谱成分来自两个恒星目标;两次观测的视向速度相差约20.3 km·s-1,观测时隔3 d,说明其绕转周期小于6 d。考虑到多个目标成分在同一条光谱上同时出现的条件极其严苛:光谱型差异较大且亮度(流量)在同一尺度上,对其光谱成分、成像、光变等内容进行了深入分析。从ZTF测光的图像序列中,可以检测到目标轮廓的尺寸呈现周期性变化,而在ASAS-SN和ZTF光变曲线上,并未发现明显的周期性变化规律;同时,由于两个天体距离极近或投影掩盖,从SDSS、2MASS测光图像上,呈现出点源的特征(边界稍显不规则),无法分辨双星目标,因此该双星系统的两个恒星之间可能轨道较为紧密,半径较小;在其光谱上呈现Balmer弱发射线(Hα、Hβ、Hδ、Hγ)和禁线([NII]λ6550、[SII]λλ6718,6733、[OII]λ3728)且目标未在行星状星云或HII区域,推测是由伴星相互作用产生的潮汐效应和物质交换,从而对恒星表面和大气层带来Compact binary systems usually have faster orbital motion,more frequent light variation effects,and the rapid evolution of companion stars,so they are important for studying interstellar physical processes and stellar evolution.Photometric images and light curves are the most common approaches to identifying binary stars.Suppose the current observation technology cannot distinguish binary objects'brightness and position difference.In that case,the spectral type is also one of the important methods used to distinguish the composition of the companion star.This paper uses the spectral binary star analysis method based on a rough set and cluster voting mechanism to analyze the spectral characteristics and identify the outlier LAMOST J051402.68+172659.7.First,for the spectral binary stars(DoubleStar)released by LAMOST DR10,human inspecting was conducted on the 17 target spectra with the lowest number of votes in its multiple clustering results.In addition to the low signal-to-noise ratio of most spectra,the two observed spectra of LAMOST J051402.68+172659.7 show great difference;For the two observations of the target,its spectrum once presents F-type and once presents F+M type.After excluding the pollution of neighboring optical fibers and other targets in the target's environment,it is determined that the real components of the target are displayed in the two observation spectra,indicating that the two spectral components come from two stellar targets.The radial velocity difference between the two observations is about 20.3 km·s-1,and the observation interval is 3 days,indicating that the rotation period is less than 6 days.Considering that the conditions for the simultaneous occurrence of multiple target components in the same spectrum are extremely strict,the spectral types are very different,and the luminance(flow)is on the same scale,the spectral components,imaging,and light variation are analyzed in depth in this paper.From the image sequence of ZTF photometry,it can be detected that the size of the target con

关 键 词：光谱双星 光变 恒星活动 郭守敬望远镜(LAMOST) 

分 类 号：P14[天文地球—天体物理]