Publications of the MPIfR
Optical & Infrared
Interferometry Group
F. 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 (invited paper)
Disentangling the wind and the disk in the
close surrounding of the young stellar object MWC297 with AMBER/VLTI
"ESO Astrophysics Symposia"
Proceedings of the ESO Workshop: "The power of
optical/IR interferometry: recent scientific results and 2nd generation
VLTI instrumentation"
April 4-8, 2005 in Garching, Germany
pg.255-262 (2008)
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 line at 2.1656µm. The object has not only been resolved in the
continuum
with a visibility of 0.50±0.10, but also in the Br 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.
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