  The star S CrA is a tight visual binary consisting of two classical T Tauri
stars, both with outstanding spectral characteristics and brightness
variations. High-resolution spectra were collected at ESO and photometric
observations with the SMARTS telescope.
  Both stars undergo large variation in brightness caused mainly by variable
foreground extinction. From the stellar parameters we conclude that the two
stars are remarkably similar, and that S CrA can be regarded as a T Tauri twin.
Rotational periods and inclinations are also similar. The stars differ,
however, in terms of degree of veiling and emission line profiles.
  We compared observed Balmer emission line profiles with models including
magnetospheric accretion and a disk wind. We found a good match between
observed signatures of accreting gas, wind features, and rotational velocities
with those resulting from our modelling for inclinations of around 65 degrees.
At this orientation the trajectories of infalling gas just above the stellar
surfaces are parallel to the line-of-sight, and accordingly we observe extended
red-shifted absorption components extending to + 380 km/s, the estimated
free-fall velocity at the surface. However, our so derived inclinations differ
from those derived from interferometric near-infrared spectroscopy, and we
discuss possible causes for this puzzling discrepancy.
