摘要
We present optical spectroscopic observations of SS 433 during different precessional and orbital phases.Our 2004,2007 and 2008 data provide us a good chance to study the variability of the Hα line at different orbital phases for nearly the same disk inclination.The data show that the Hα of SS 433 usually had a symmetric profile between orbital phases 0.25-0.75,while an asymmetric structure with a strong red peak was observed for other orbital phases.We suggest that the orbital variability of Hα emission is connected with accretion flow from the donor star to the accretion disk.In addition,we attribute the dramatic increase of Hα emission during our 2007 observational run,which had a time scale of one day,to the emergence of strong jets.
We present optical spectroscopic observations of SS 433 during different precessional and orbital phases.Our 2004,2007 and 2008 data provide us a good chance to study the variability of the Hα line at different orbital phases for nearly the same disk inclination.The data show that the Hα of SS 433 usually had a symmetric profile between orbital phases 0.25-0.75,while an asymmetric structure with a strong red peak was observed for other orbital phases.We suggest that the orbital variability of Hα emission is connected with accretion flow from the donor star to the accretion disk.In addition,we attribute the dramatic increase of Hα emission during our 2007 observational run,which had a time scale of one day,to the emergence of strong jets.
作者
LI Hui1,2 & YAN JingZhi1,3 1 Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China
2 Graduate University of Chinese Academy of Sciences,Beijing 100049,China
3 Service d’Astrophysique,CEA Saclay and University Paris Diderot,91191 Gif-sur-Yvette,France
基金
supported by the National Basic Research Program of China (Grant No. 2009CB824800)
the Natural Science Foundation of China (Grant Nos. 10873036 and 10673032)
