The observation and theoretical study of massive magnetized white dwarfs is one of the most important topics in the field of astronomy. This paper aims to obtain a coupled magneto-thermal evolution model of magnetized white dwarfs (B-WDs). As a fiducial model, we choose a non-magnetized WD with a baryonic mass M 0 = 1.37 M ⊙ (M ⊙ is the solar mass) for comparison with the magnetized cases. Firstly, we give an overview of the WD cooling, then study the equation of the state of a B-WD. We find that the WD mass increases with magnetic field strength B, while its radius decreases with B, and the minimum of B required to reach the Chandrasecka limit is about 3.2 × 10 14 G. Finally, by introducing the magnetic-to-thermal conversion coefficient ξ, and taking the temperature effect on the stellar radius into consideration, we calculate the luminosities of thermal photons L ph and surface effective temperature, T eff due to Ohmic dissipation for B-WDs. According to our calculations, magnetic field decay can definitely maintain a long-term thermal evolution for massive B-WDs. This study will be useful for the study of internal thermal evolution and internal stability of B-WDs in the future.
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