TT Arietis: Spectroscopy and Photometry

We report the photometry and spectroscopy of TT Arietis around the turn of the millennium, when the nova-like variable is in high state. A positive superhump since 1997 still exists. A more precise orbital period than before, 0:13755040+/-1.7x10(-7) days, is established. The intensity of the Balmer emission core is found to modulate at the superhump period rather than the orbital period and 180degrees out of phase with continuum. The intensity of Balmer absorption wings is approximately proportional to the continuum flux. The correlation between Balmer lines and continuum provides a new clue to the study of sources of continuum and emission lines. The mass ratio of the binary is found to be in the range of 0.19+/-0.04, which lends strong support to the proposition that superhumps arise from the inner Lindblad 3: 1 resonance in TT Ari, as in superoutbursts of SU UMa stars.