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Debris disks are the intrinsic by-products of the star and planet formationprocesses. Most likely due to instrumental limitations and their naturalfaintness, little is known about debris disks around low-mass stars, especiallywhen it comes to spatially resolved observations. We present new VLT/SPHEREIRDIS Dual-Polarization Imaging (DPI) observations in which we detect the dustring around the M2 spectral type star TWA\,7. Combined with additional AngularDifferential Imaging observations we aim at a fine characterization of thedebris disk and setting constraints on the presence of low-mass planets. Wemodel the SPHERE DPI observations and constrain the location of the small dustgrains, as well as the spectral energy distribution of the debris disk, usingthe results inferred from the observations, and perform simple N-bodysimulations. We find that the dust density distribution peaks at 25 au, with avery shallow outer power-law slope, and that the disk has an inclination of 13degrees with a position angle of 90 degrees East of North. We also report lowsignal-to-noise detections of an outer belt at a distance of ~52 au from thestar, of a spiral arm in the Southern side of the star, and of a possible dustyclump at 3.9 au. These findings seem to persist over timescales of at least ayear. Using the intensity images, we do not detect any planets in the closevicinity of the star, but the sensitivity reaches Jovian planet mass upperlimits. We find that the SED is best reproduced with an inner disk at 7 au andanother belt at 25 au. We report the detections of several unexpected featuresin the disk around TWA\,7. A yet undetected 100 M$_\oplus$ planet with asemi-major axis at 20-30 au could possibly explain the outer belt as well asthe spiral arm. We conclude that stellar winds are unlikely to be responsiblefor the spiral arm.

Resolving faint structures in the debris disk around TWA7