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Wind and disk interaction in MWC 297
Monday 11 July 2005, by Fabien Malbet


Disentangling the wind and the disk in the close surrounding of the young stellar object MWC297 with AMBER/VLTI

Fabien Malbet, M. Benisty, W.J. De Wit, S. Kraus, A. Meilland, F. Millour, E. Tatulli, J.-P. Berger, O. Chesneau, K.-H. Hofmann, A. Isella, R. Petrov, T. Preibisch, P. Stee, L. Testi, G. Weigelt and the AMBER consortium.

To be published in the Proceedings of the ESO Workshop on "The Power of Optical/IR Interferometry: Recent Scientific Results and 2nd Generation VLTI Instrumentation", held in Garching, Germany, 4-8 April 2005

Available as the astro-ph/0507226 preprint and also on the HAL preprint server.

Abstract: 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.


MWC 297 - ESO preprint





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