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Circumstellar disks and outflows play a fundamental role in star formation.Infrared spectro-interferometry allows the inner accretion-ejection region tobe resolved. We measured interferometric visibilities, wavelength-differentialphases, and closure phases of MWC 297 with a spectral resolution of 12000. Tointerpret our MWC 297 observations, we employed disk-wind models. The measuredcontinuum visibilities confirm previous results that the continuum-emittingregion of MWC 297 is remarkably compact. We derive a continuum ring-fit radiusof ~2.2 mas (~0.56 AU at a distance of 250 pc), which is ~5.4 times smallerthan the 3 AU dust sublimation radius expected for silicate grains (in theabsence of radiation-shielding material). The strongly wavelength-dependent andasymmetric Br gamma-emitting region is more extended (~2.7 times) than thecontinuum-emitting region. At the center of the Br gamma line, we derive aGaussian fit radius of ~6.3 mas HWHM (~1.6 AU). To interpret the observations,we employ a magneto-centrifugally driven disk-wind model consisting of anaccretion disk, which emits the observed continuum radiation, and a disk wind,which emits the Br gamma line. The calculated wavelength-dependent modelintensity distributions and Br gamma line profiles are compared with theobservations (i.e., K-band spectrum, visibilities, differential phases, andclosure phases). The closest fitting model predicts a continuum-emitting diskwith an inner radius of ~0.3 AU and a disk wind ejection region with an innerradius of ~0.5 AU (~17.5 stellar radii). We obtain a disk-wind half-openingangle (the angle between the rotation axis and the innermost streamline of thedisk wind) of ~80 degrees, which is larger than in T Tau models, and a diskinclination angle of ~20 degrees (i.e., almost pole-on).

VLTI/AMBER spectro-interferometry of the Herbig Be star MWC 297 with spectral resolution 12 000