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Resolving the dusty circumstellar environment of the A[e] supergiant HD 62623 with the VLTI/MIDI

Published online by Cambridge University Press:  12 July 2011

Antony Meilland ,
Sameer Kanaan ,
Marcelo Borges Fernandes ,
Olivier Chesneau ,
Florentin Millour ,
Philippe Stee  and
Bruno Lopez
Antony Meilland
Affiliation:
Max-Planck Institut fr Radioastronomie, Bonn, Germany
Sameer Kanaan
Affiliation:
Universidad de Valparaso, Chile
Marcelo Borges Fernandes
Affiliation:
Observatorio Nacional, Rio de Janeiro, Brazil
Olivier Chesneau
Affiliation:
UMR Fizeau, UNS-OCA-CNRS, Nice, France
Florentin Millour
Affiliation:
Max-Planck Institut fr Radioastronomie, Bonn, Germany UMR Fizeau, UNS-OCA-CNRS, Nice, France
Philippe Stee
Affiliation:
UMR Fizeau, UNS-OCA-CNRS, Nice, France
Bruno Lopez
Affiliation:
UMR Fizeau, UNS-OCA-CNRS, Nice, France
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Abstract

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HD 62623 is one of the very few A-type supergiants showing the B[e] phenomenon. We studied the geometry of its circumstellar envelope in the mid-infrared using the VLTI/MIDI instrument. Using the radiative transfer code MC3D, we managed to model it as a dusty disk with an inner radius of 3.85 AU, an inclination angle of 60°, and a mass of 2 × 10−7M⊙. It is the first time that the dusty disk inner rim of a supergiant star exhibiting the B[e] phenomenon is significantly constrained. The inner gaseous envelope likely contributes up to 20% to the total N band flux and acts like a reprocessing disk. Finally, the hypothesis of a stellar wind deceleration by the companion gravitational effect remains the most probable case since the bi-stability mechanism is not efficient for this star.

Keywords

techniques: high angular resolutionstars: emission-lineBestars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 406 - 407
Copyright
Copyright © International Astronomical Union 2011

References

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