This paper investigates the properties of accretion disks around regular black hole (RBH) solutions derived from non-linear electrodynamics (NLED). The study focuses on the Dymnikova and Fan-Wang spacetimes, which are spherically symmetric and static, and examine the characteristics of accretion disks in these spacetimes. The research employs the Novikov-Thorne-Page thin accretion disk model to analyze the properties of accretion disks, including the radius of the innermost stable circular orbit (ISCO), radiant energy, temperature, and conversion efficiency of accretion mass into radiation. The findings are compared with those obtained in the Schwarzschild black hole case, revealing significant modifications in the overall spectral properties. Specifically, the study observes an increase in the energy emitted from the disk surface, resulting in higher temperatures for the accretion disks under certain values of the free parameters. Consequently, the efficiency of mass conversion into radiation is enhanced compared to the Schwarzschild spacetime. The results indicate that the introduction of non-zero free parameters in the Dymnikova and Fan-Wang metrics leads to a reduction in the corresponding ISCOs, and an increase in the energy emitted from the disk surface. Additionally, the study finds that the temperature of the accretion disk around RBHs increases with certain values of the free parameters. The results also show that the efficiency of mass conversion into radiation is higher for the Dymnikova and Fan-Wang BHs compared to the Schwarzschild spacetime. The study concludes that the particular solutions obtained from NLED may be more efficient in converting mass into radiation than Schwarzschild BHs, suggesting how future explorations can check whether a given compact object can be described by such solutions or not. The paper also discusses the implications of these findings for future research on rotating RBHs, the impact of magnetic fields and dark matter on the physical characteristics of the accretion disk, and the potential deviations from the current approach.This paper investigates the properties of accretion disks around regular black hole (RBH) solutions derived from non-linear electrodynamics (NLED). The study focuses on the Dymnikova and Fan-Wang spacetimes, which are spherically symmetric and static, and examine the characteristics of accretion disks in these spacetimes. The research employs the Novikov-Thorne-Page thin accretion disk model to analyze the properties of accretion disks, including the radius of the innermost stable circular orbit (ISCO), radiant energy, temperature, and conversion efficiency of accretion mass into radiation. The findings are compared with those obtained in the Schwarzschild black hole case, revealing significant modifications in the overall spectral properties. Specifically, the study observes an increase in the energy emitted from the disk surface, resulting in higher temperatures for the accretion disks under certain values of the free parameters. Consequently, the efficiency of mass conversion into radiation is enhanced compared to the Schwarzschild spacetime. The results indicate that the introduction of non-zero free parameters in the Dymnikova and Fan-Wang metrics leads to a reduction in the corresponding ISCOs, and an increase in the energy emitted from the disk surface. Additionally, the study finds that the temperature of the accretion disk around RBHs increases with certain values of the free parameters. The results also show that the efficiency of mass conversion into radiation is higher for the Dymnikova and Fan-Wang BHs compared to the Schwarzschild spacetime. The study concludes that the particular solutions obtained from NLED may be more efficient in converting mass into radiation than Schwarzschild BHs, suggesting how future explorations can check whether a given compact object can be described by such solutions or not. The paper also discusses the implications of these findings for future research on rotating RBHs, the impact of magnetic fields and dark matter on the physical characteristics of the accretion disk, and the potential deviations from the current approach.