活动色球双星HR1099近红外分光光度观测  

Infrared Spectrophotometry of the Chromospherically Active Binary HR 1099

作　　者：翟迪生[1] 张效愚 王俊杰[1] 

机构地区：[1]中国科学院北京天文台

出　　处：《天体物理学报》1995年第2期152-162,共11页

基　　金：国家自然科学基金;国家攀登计划资助

摘　　要：本文发表了强活动色球双星ＨＲ１０９９（＝Ｖ７１１Ｔａｕ）在１９８９年１２月特大能量白光耀发前后的近红外分光光度观测结果，给出该星从２．３－４．１μｍ首次ＣＶＦ低色散光谱，以及耀发前后的变化；计算了同期观测到的子星表面黑子的影响，给出双星黑体近似辐射能谱，并与多波段测光以及ＩＲＡＳ观测作了对比，揭示了该双星有很强的星周物质的２．３μｍ发射带和３．１μｍ波段吸收带特征，本文对可能的星周物质成分和分布亦作了初步讨论。Spectrophotometry in the near-infrared(2.3-4.1μm) was carried out for the chromospherically active binary system HR 1099.The observations were made by using the Circular Variable Filter at the 1.26 m telescope of Beijing Observatory on 1989 December 13/14 and 15/16, immediately before and after the giant optical flares on 1989 December 14/15. Considering the influence of starspots of the secondary obtained from optical distortion wave, the theoretical energy distribution of the black-body approximation from 0.35 to 25μm is constructed for the binary system and compared with the observed CVF spectra as well as the published UBVRIJHK and IRAS's 12 and 25μm observations. It turns out that there are strong 2.3 μm emission and 3. 1 μm absorption bands with half width about 0.4 μm for each and both bands suffered obvious changes after the flares, which indicates the existence of the circulnstellar contribution of the binary system. However, the unusual IR 2.3 and 3.1μm features of HR 1099, the first discovery among the RS CVn systems,cannot be simply explained by the thermal emission of dust shell as it could be the case in cool giant stars.The probable components and distributions of the circumstellar matter are discussed,which call for further observational evidences.

关 键 词：双星 红外分光光度 星周物质 活动色球 

分 类 号：P153[天文地球—天文学]