  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
+- 0.03 mas (corresponding to 0.095 +- 0.018 AU for a distance of 130 pc) and
0.85 +- 0.07 mas (0.111 +- 0.026 AU), respectively. This K-band radius is
approximately two times larger than the dust sublimation radius of ~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 ~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 ~0.11 AU. The narrow extension of the inner
temperature-gradient disk component implies that there is a hot inner rim.
