Be星光谱和近红外光度观测  

Spectroscopic and Near Infrared Photometric Observations of Be Stars

作　　者：杭恒荣 夏剑萍 陈亚峰 常进 

出　　处：《紫金山天文台台刊》1994年第1期77-77,共1页

摘　　要：Equivalent widths (EW) of Hα emission lines and JHK magnitudes for 24 Be Stars were measured. Spectroscopic and near infrared photometric Observations were made with 216 cm telescope and 126 cm telescope separately at Beijing Astronomical Observatory in the autumn of 1992. Some additional apectra were obtained with 100 cm telescope at Yunnan Astronomical Observatory in January 1993.As a preliminary analysis of the data, the correlation between EW of Hαand colour index J-K of Be Stars was investigated. The EW as a function of J-K were plotted. It is shown that the EW of Hα emission line is proportional to J-K quite well for Be Stars we observed, except two stars: KX And and LSI 61 °303, of which the infrared excess are too large, ΔEW /Δ(J-K) is equal to 100 A / magnitude, this correlation indicates that both infrared excess and Hα emission originate in a commom region of envelope around Be stars.Equivalent widths (EW) of Hα emission lines and JHK magnitudes for 24 Be Stars were measured. Spectroscopic and near infrared photometric Observations were made with 216 cm telescope and 126 cm telescope separately at Beijing Astronomical Observatory in the autumn of 1992. Some additional apectra were obtained with 100 cm telescope at Yunnan Astronomical Observatory in January 1993. As a preliminary analysis of the data, the correlation between EW of Hαand colour index J-K of Be Stars was investigated. The EW as a function of J-K were plotted. It is shown that the EW of Hα emission line is proportional to J-K quite well for Be Stars we observed, except two stars: KX And and LSI 61 °303, of which the infrared excess are too large, ΔEW /Δ(J-K) is equal to 100 A / magnitude, this correlation indicates that both infrared excess and Hα emission originate in a commom region of envelope around Be stars.

关 键 词：BE星 光谱 近红外光度 

分 类 号：P145.4[天文地球—天体物理]