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Recent observations in extreme-ultraviolet (EUV) wavelengths reveal an EUVlate phase in some solar flares, which is characterized by a second peak in thewarm coronal emissions (about 3 MK) occurring several tens of minutes to a fewhours after the corresponding main flare peak. We aim to clarify the physicalorigin of an atypical plateau-like EUV late phase in an X1.8-class solar flareoccurring on 2011 September 7 from active region (AR) 11283. We firstcharacterize the plateau-like late phase using EUV Variability Experiment (EVE)full-disk integrated irradiance observations and Atmospheric Imaging Assembly(AIA) spatially-resolved imaging observations on board the Solar DynamicsObservatory (SDO). Then we perform a nonlinear force-free-field (NLFFF)extrapolation, from which a filament-hosting magnetic flux rope (MFR) isrevealed. The eruption of the MFR is tracked both in the plane of the sky (POS)and along the line of sight (LOS) through visual inspection and spectralfitting, respectively. Finally, we carry out differential emission measure(DEM) analysis to explore the thermodynamics of the late-phase loops. The MFRshows a non-radial eruption from a fan-spine magnetic structure. The eruptionof the MFR and its interaction with overlying arcades invoke multiple magneticreconnections, which are responsible for the production of different groups oflate-phase loops. Afterwards, the late-phase loops enter a long-lasting coolingstage, appearing sequentially in AIA passbands of decreasing responsetemperatures. Due to their different lengths, the different groups oflate-phase loops cool down at different cooling rates, which makes their warmcoronal emission peaks temporally separated from each other. Combing theemissions from all late-phase loops together, an elongated plateau-like latephase is formed.

An Atypical Plateau-like Extreme-ultraviolet Late-phase Solar Flare Driven by the Non-radial Eruption of a Magnetic Flux Rope