IU Leo was first identified as a cataclysmic variable star in 2006. Based on image data and a distance value, we derived that the circumbinary envelope of IU Leo was ∼3745 au on the optical band. According to the multi-band photometric data, we calculated a Teff of a few hundred Kelvin for the circumbinary envelope of IU Leo. We reviewed the physical parameters of IU Leo and simulated the evolution process using a stellar evolution code MESA with M1 = 0.982 M⊙, M2 = 0.835 M⊙, and an orbital period of 0.376308 day. The evolved other parameters are basically consistent with the parameters in the literatures. Based on the quiescence Kepler Mission 2.0 light curve, the quiescence Transiting Exoplanet Survey Satellite light curve, and 89 Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) medium resolution spectra, we derived an orbital period of 0.376307 ± 0.000004 days, 0.3762 ± 0.0001 days, and 0.3763 day for IU Leo respectively. These orbital periods are basically consistent with the results of previous studies. According to the light curve of IU Leo from the American Association of Variable Star Observers, we reported three new outburst spectra from the LAMOST low resolution catalogue with a part of the Balmer emission lines overlap on their absorption lines. Many H, He, C, N, O, Na, Mg, Si, and Ca neutral and ionized lines are identified, which are produced by different mechanisms. In the future, we will conduct more comprehensive and in-depth research on CVs based on multi-band photometric and spectroscopic data.