对矮新星EG Cancri 1996年爆发的研究  

OPTICAL STUDY OF EG CANCRI OUTBURST IN 1996

作　　者：刘武[1] 胡景耀[1] 李宗云[2] 曹莉[1] 

机构地区：[1]中国科学院北京天文台,北京100080 [2]南京大学天文系,南京210093

出　　处：《中国科学院上海天文台年刊》1998年第19期239-247,共9页Annals Shanghai Astronomical Observatory Chinese Academy of Sciences

摘　　要：给出了矮新星EGCue在1996～1997年爆发期间的光变曲线和光谱。光变曲线显示了它在下降过程中有较大的亮度波动及mini－outburst。光谱从爆发时的蓝吸收谱演化为宁静期有双峰的巴尔末发射线谱。从宁静期的CCD快速测光，得到它的轨道周期为0．0575±0．0026天。Matsumoto[1]观测到了爆发期的superhump。由于EGCnc具有大变幅爆发（≈7mag），缓慢下降，爆发间隔长（19年），极短轨道周期和superhump等特征，我们认为这是一颗较少见的WZSge型矮新星。The optical light curve of EG Cancri during its outburst in 1996~1997 were presented.It has displayed some brightness fluctuations in the phase of decline. Mini - outbursts were detected. Optical spectra obtained during the decline showed it to be a dwarf nova on account of its broad absorption lines superimposed on a blue continuum. Optical spectra near minimum brightness revealed doubled Balmer lines in emission, over broad absorptions, but no HeII4686. An additional heating presented in the last stage of decline. CCD time - resolved photometry showed a possible orbital period 0. 0575 ±0. 0026 day. Superhumps were observed during outburst by Matsumoto(1996). EG Cancri is a CVs that has large - amplitude outburst (7mag), slow decline from outburst, long intervals between outburst and short period. From above properties, we classify the CVs, EG Cancri, as a WZ Sge type DN is plausible.

关 键 词：激变变星 矮新星 EGCancri 光变曲线 光谱 

分 类 号：P145.2[天文地球—天体物理]