  The young stellar object MWC297 is a B1.5Ve star exhibiting strong hydrogen
emission lines. This object has been observed by the AMBER/VLTI instrument in
2-telescope mode in a sub-region of the K spectral band centered around the Br
gamma line at 2.1656 microns. The object has not only been resolved in the
continuum with a visibility of 0.50+/-0.10, but also in the Br gamma line,
where the flux is about twice larger, with a visibility about twice smaller
(0.33+/-0.06). The continuum emission is consistent with the expectation of an
optically thick thermal emission from dust in a circumstellar disk. The
hydrogen emission can be understood by the emission of a halo above the disk
surface. It can be modelled as a latitudinal-dependant wind model and it
explains the width, the strength and the visibibility through the emission
lines. The AMBER data associated with a high resolution ISAAC spectrum
constrains the apparent size of the wind but also its kinematics.
