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Hydrodynamical simulations of a compact source scenario for G2

Published online by Cambridge University Press:  22 May 2014

A. Ballone ,
M. Schartmann ,
A. Burkert ,
S. Gillessen ,
R. Genzel ,
T. K. Fritz ,
F. Eisenhauer ,
O. Pfuhl  and
T. Ott
A. Ballone
Affiliation:
University Observatory Munich, Scheinerstraße 1, D-81679 München, Germany email: aballone@mpe.mpg.de Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
M. Schartmann
Affiliation:
University Observatory Munich, Scheinerstraße 1, D-81679 München, Germany email: aballone@mpe.mpg.de Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
A. Burkert
Affiliation:
University Observatory Munich, Scheinerstraße 1, D-81679 München, Germany email: aballone@mpe.mpg.de Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany Max-Planck Fellow
S. Gillessen
Affiliation:
Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
R. Genzel
Affiliation:
Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
T. K. Fritz
Affiliation:
Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
F. Eisenhauer
Affiliation:
Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
O. Pfuhl
Affiliation:
Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
T. Ott
Affiliation:
Max-Planck-Institute for Extraterrestrial Physics, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany
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Abstract

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The origin of the dense gas cloud “G2” discovered in the Galactic center (Gillessen et al. 2012) is still a debated puzzle. G2 might be a diffuse cloud or the result of an outflow from an invisible star embedded in it. We present here detailed simulations of the evolution of winds on G2's orbit. We find that the hydrodynamic interaction with the hot atmosphere present in the Galactic center and the extreme gravitational field of the supermassive black hole must be taken into account when modeling such a source scenario. We also find that in this scenario most of the Brγ luminosity is expected to come from the highly filamentary densest shocked wind material. G2's observational properties can be used to constrain the properties of the outflow and our best model has a mass outflow rate of Ṁw=8.8 × 10−8 M⊙ yr−1 and a wind velocity of vw = 50 km s−1. These values are compatible with those of a young TTauri star wind, as already suggested by Scoville & Burkert (2013).

Keywords

Galaxy: centerindividual (Sgr A*, G2) — methods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S303: The Galactic Center: Feeding and Feedback in a Normal Galactic Nucleus , October 2013 , pp. 307 - 311
Copyright
Copyright © International Astronomical Union 2014 

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