Super-Eddington AGNs are the most powerful accretion systems in the Universe. There are super-Eddington NLS1s with masses less than 1.E7 Msun, which are well known for exhibiting weak [O III], strong Fe II, and a significant soft X-ray excess. Besides, there are weak-line quasars (WLQs) with masses bigger than 1.E8 Msun, which are characterized by notably weak high-ionization UV emission lines, such as C IV and N V. Both types of systems also exhibit strong X-ray variability. In this talk, I will present a unique NLS1 population that possesses properties similar to both NLS1s and WLQs, including NLS1-like optical emission lines, WLQ-like UV emission lines, and drastic X-ray variability. This a representative population of super-Eddington AGNs, which we termed "Weak-Line" Seyferts. I will discuss how the evolution of the super-Eddington accretion flow, in terms of black hole mass and accretion rate, can help us understand these three types of super-Eddington AGNs