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

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: weigelt@mpifr.de
² Pulkovo Observatory of RAS, Pulkovskoe shosse 65, St. Petersburg 196140, Russia
³ V.V. Sobolev Astronomical Institute, St. Petersburg University, St. Petersburg, Russia
⁴ Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USA
⁵ University of North Carolina at Greensboro, PO Box 26170, Greensboro, NC 27402, USA
⁶ INAF-Osservatorio Astrofisico di Arcetri, Istituto Nazionale di Astrofisica, Largo E. Fermi 5, 50125 Firenze, Italy
⁷ Deutsches Zentrum für Luft- und Raumfahrt e.V., Königswinterer Str. 522-524, 53227 Bonn, Germany
⁸ Laboratoire H. Fizeau, University of Nice Sophia Antipolis, CNRS, OCA, Parc Valrose, 06108 Nice, France
⁹ Laboratoire d’Astrophysique de Grenoble, UMR 5571 Université Joseph Fourier/CNRS, BP 53, 38041 Grenoble Cedex 9, France

Received: 2 September 2010
Accepted: 27 November 2010

Abstract

Context. Circumstellar disks and outflows play a fundamental role in star formation. Infrared spectro-interferometry allows the inner accretion-ejection region to be resolved.

Aims. We study the disk and Brγ-emitting region of MWC 297 with high spatial and spectral resolution and compare our observations with disk-wind models.

Methods. We measured interferometric visibilities, wavelength-differential phases, and closure phases of MWC 297 with a spectral resolution of 12 000. To interpret our MWC 297 observations, we employed disk-wind models.

Results. The measured continuum visibilities confirm previous results that the continuum-emitting region of MWC 297 is remarkably compact. We derive a continuum ring-fit radius of  ~2.2 mas (~0.56 AU at a distance of 250 pc), which is  ~5.4 times smaller than the 3 AU dust sublimation radius expected for silicate grains (in the absence of radiation-shielding material). The strongly wavelength-dependent and asymmetric Brγ-emitting region is more extended (~2.7 times) than the continuum-emitting region. At the center of the Brγ line, we derive a Gaussian 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 an accretion disk, which emits the observed continuum radiation, and a disk wind, which emits the Brγ line. The calculated wavelength-dependent model intensity distributions and Brγ line profiles are compared with the observations (i.e., K-band spectrum, visibilities, differential phases, and closure phases). The closest fitting model predicts a continuum-emitting disk with an inner radius of  ~0.3 AU and a disk wind ejection region with an inner radius of  ~ 0.5 AU (~17.5 stellar radii). We obtain a disk-wind half-opening angle (the angle between the rotation axis and the innermost streamline of the disk wind) of  ~80°, which is larger than in T Tau models, and a disk inclination angle of  ~20° (i.e., almost pole-on).

Conclusions. Our observations with a spectral resolution of 12 000 allow us to study the AU-scale environment of MWC 297 in  ~10 different spectral channels across the Brγ emission line. We show that the K-band flux, visibilities, and remarkably strong phases can be explained by the employed magneto-centrifugally driven disk wind model.