This article reports the spectral behavior of CH Cygni, using data obtained in October 2005 and June 2006. In these epochs, CH Cygni showed emission lines of H I, Fe II, [Fe II], [O III], [N II], [Ne III] and [S II]. Many of these lines were more enhanced since 2004. The underlying M-type spectrum was removed to get the intrinsic emission profile, and the resulting profiles were deconvoluted into several Gaussian components. Also, the radial velocities for all the lines that appeared in these spectra of CH Cygni were measured. The resultant lines were compared with each other and with those obtained in 2004; the findings are explained in terms of an accretion disk and jets.

변광성 TU UMi의 변광 유형의 분류를 위하여 소백산 천문대 0.6m광학 망원경과 2K CCD 카메라를 이용하여 B, V, I 필터를 이용한 시계열 측광 관측을 수행하였다. 변광성의 분류를 위하여 V 필터와 I 필터로부터 얻은 광도 곡선의 진폭의 비(δi/δv), 색의 변화(δ(b-v), δ(v-i))로 부터 TU UMi가 W UMa형 식쌍성임을 확인하였으며, 우리의 관측 자료에서 2개의 극심 시각(UJD 2453848.04456, HJD 2453848.23088)을 구하였고, 새로운 광도 요소(Min I=HJD 2452500.1344+0.37708907×E)를 결정하였다.