We propose a new method to reconstruct the structure of accretion disks in dwarf novae using multi-band light curves of early superhumps .
Our model assumes that early superhumps are caused by the rotation effect of non-axisymmetrically flaring disks .
We have developed a Bayesian model for this reconstruction , in which a smoother disk-structure tends to have a higher prior probability .
We analyzed simultaneous optical and near-infrared photometric data of early superhumps of the dwarf nova , V455 And using this technique .
The reconstructed disk has two flaring parts in the outermost region of the disk .
These parts are responsible for the primary and secondary maxima of the light curves .
The height-to-radius ratio is h / r = 0.20 — 0.25 in the outermost region .
In addition to the outermost flaring structures , flaring arm-like patterns can be seen in an inner region of the reconstructed disk .
The overall profile of the reconstructed disk is reminiscent of the disk structure that is deformed by the tidal effect .
However , an inner arm-like pattern , which is responsible for the secondary minimum in the light curve , can not be reproduced only by the tidal effect .
It implies the presence of another mechanism that deforms the disk structure .
Alternatively , the temperature distribution of the disk could be non-axisymmetric .
We demonstrate that the disk structure with weaker arm-like patterns is optimal in the model including the irradiation effect .
However , the strongly irradiated disk gives quite blue colors , which may conflict with the observation .
Our results suggest that the amplitude of early superhumps depends mainly on the height of the outermost flaring regions of the disk .
We predict that early superhumps can be detected with an amplitude of > 0.02 mag in about 90 % of WZ Sge stars .