Spectral variations of carbon stars based on ISO SWS data  

作　　者：Xiao-Hong Yang Pei-Sheng Chen 

机构地区：[1]Department of Physics, Chongqing University, Chongqing 400044, China [2]National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China

出　　处：《Research in Astronomy and Astrophysics》2009年第12期1359-1367,共9页天文和天体物理学研究（英文版）

基　　金：supported by the National Natural Science Foundation of China(Grant No.10803023);supported by the Natural Science Foundation Project of CQ CSTC(No.2008BB0153)

摘　　要：We investigate the spectral variations of seven carbon stars in the infrared using ISO SWS spectral data. Continuum variations of those carbon stars show that during the central star pulsations when carbon stars become fainter in the infrared, their ISO SWS spectra become redder and the near-IR temperature （Tnir） decreases. When carbon stars become brighter in the infrared, their ISO SWS spectra become bluer and Tnir increases. Furthermore, it is found that the shorter 1abe wavelength of spectral features, such as the 2.48＋2.58 （C2H2＋HCN＋CO＋C2）, 3.05 （C2H2＋HCN） and 3.90 （C2H2） μm features, is, the better the correlation of their relative integrated fluxes with the fluxes of the continuum is. The changes of the 5.2 （C3）, 11.30 （SIC） and 13.70 （C2H2）μm features do not obviously correlate with the fluxes of the continuum.We investigate the spectral variations of seven carbon stars in the infrared using ISO SWS spectral data. Continuum variations of those carbon stars show that during the central star pulsations when carbon stars become fainter in the infrared, their ISO SWS spectra become redder and the near-IR temperature （Tnir） decreases. When carbon stars become brighter in the infrared, their ISO SWS spectra become bluer and Tnir increases. Furthermore, it is found that the shorter 1abe wavelength of spectral features, such as the 2.48＋2.58 （C2H2＋HCN＋CO＋C2）, 3.05 （C2H2＋HCN） and 3.90 （C2H2） μm features, is, the better the correlation of their relative integrated fluxes with the fluxes of the continuum is. The changes of the 5.2 （C3）, 11.30 （SIC） and 13.70 （C2H2）μm features do not obviously correlate with the fluxes of the continuum.

关 键 词：stars： AGB and post-AGB -- stars： mass loss -- infrared： stars 

分 类 号：TQ116.3[化学工程—无机化工] TP75[自动化与计算机技术—检测技术与自动化装置]