Disentangling the wind and the disk in the close surrounding of the young stellar object MWC 297 with AMBER/VLTI

被引:0
|
作者
Malbet, F. [1 ]
Benisty, M. [1 ]
de Wit, W. J. [1 ]
Kraus, S. [5 ]
Meilland, A. [2 ]
Millour, F. [1 ,3 ]
Tatulli, E. [1 ]
Berger, J. -P. [1 ]
Chesneau, O. [2 ]
Hofmann, K. -H. [5 ]
Isella, A. [4 ]
Petrov, R. [3 ]
Preibisch, T. [5 ]
Stee, P. [2 ]
Testi, L. [4 ]
Weigelt, G. [5 ]
机构
[1] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, UMR 5571, BP 53, F-38041 Grenoble 9, France
[2] Observ Cote Azur, CNRS, UMR 6203, Lab Gemini, F-06304 Nice 4, France
[3] Univ Nice, CNRS, UMR 6525, Lab Univ Astrophys Nice, F-06108 Nice 2, France
[4] Ist Nazl Astrofis, Observ Astrofis Arcetri, I-50125 Florence, Italy
[5] Max Planck Inst Radioastron, D-53121 Bonn, Germany
关键词
D O I
10.1007/978-3-540-74256-2_30
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The young stellar object MWC 297 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 mu m. 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.
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页码:255 / 262
页数:8
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