Context :

Aims : We investigate the structure of the circumstellar disk of the T Tauri star S CrA N and test whether the observations agree with the standard picture proposed for Herbig Ae stars .

Methods : Our observations were carried out with the VLTI/AMBER instrument in the H and K bands with the low spectral resolution mode .
For the interpretation of our near-infrared AMBER and archival mid-infrared MIDI visibilities , we employed both geometric and temperature-gradient models .

Results : To characterize the disk size , we first fitted geometric models consisting of a stellar point source , a ring-shaped disk , and a halo structure to the visibilities .
In the H and K bands , we measured ring-fit radii of 0.73 \pm 0.03 mas ( corresponding to 0.095 \pm 0.018 AU for a distance of 130 pc ) and 0.85 \pm 0.07 mas ( 0.111 \pm 0.026 AU ) , respectively .
This K -band radius is approximately two times larger than the dust sublimation radius of \approx 0.05 AU expected for a dust sublimation temperature of 1500 K and gray dust opacities , but approximately agrees with the prediction of models including backwarming ( namely a radius of \approx 0.12 AU ) .
The derived temperature-gradient models suggest that the disk is approximately face-on consisting of two disk components with a gap between star and disk .
The inner disk component has a temperature close to the dust sublimation temperature and a quite narrow intensity distribution with a radial extension from 0.11 AU to 0.14 AU .

Conclusions : Both our geometric and temperature-gradient models suggest that the T Tauri star S CrA N is surrounded by a circumstellar disk that is truncated at an inner radius of \approx 0.11 AU .
The narrow extension of the inner temperature-gradient disk component implies that there is a hot inner rim .