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We present results from the analysis of 2997 fundamental mode RR Lyraevariables located in the Small Magellanic Cloud (SMC). For these objectsnear-infrared time-series photometry from the VISTA survey of the MagellanicClouds system (VMC) and visual light curves from the OGLE IV survey areavailable. In this study the multi-epoch $K_{\rm s}$-band VMC photometry wasused for the first time to derive intensity-averaged magnitudes of the SMC RRLyrae stars. We determined individual distances to the RR Lyrae stars from thenear-infrared period-absolute magnitude-metallicity ($PM_{K_{\rm s}}Z$)relation, which has a number of advantages in comparison with the visualabsolute magnitude-metallicity ($M_{V}-{\rm [Fe/H]}$) relation, such as asmaller dependence of the luminosity on interstellar extinction, evolutionaryeffects and metallicity. The distances we have obtained were used to study thethree-dimensional structure of the SMC. The distribution of the SMC RR Lyraestars is found to be ellipsoidal. The actual line-of-sight depth of the SMC isin the range from 1 to 10 kpc, with an average depth of 4.3 $\pm$ 1.0 kpc. Wefound that RR Lyrae stars in the eastern part of the SMC are affected byinteractions of the Magellanic Clouds. However, we do not see a clearbimodality in the distribution of RR Lyrae stars as observed for red clump (RC)stars.

The VMC survey - XXVI. Structure of the Small Magellanic Cloud from RR Lyrae stars