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Hydrodynamical simulations of G2 interpreted as a diffuse gas cloud

Published online by Cambridge University Press:  22 May 2014

M. Schartmann ,
A. Burkert ,
A. Ballone ,
C. Alig ,
S. Gillessen ,
R. Genzel ,
F. Eisenhauer  and
T. Fritz
M. Schartmann
Affiliation:
Universitäts-Sternwarte München, Scheinerstraße 1, D-81679 München, Germany email: [email protected] Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
A. Burkert
Affiliation:
Universitäts-Sternwarte München, Scheinerstraße 1, D-81679 München, Germany email: [email protected] Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
A. Ballone
Affiliation:
Universitäts-Sternwarte München, Scheinerstraße 1, D-81679 München, Germany email: [email protected] Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
C. Alig
Affiliation:
Universitäts-Sternwarte München, Scheinerstraße 1, D-81679 München, Germany email: [email protected] Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
S. Gillessen
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
R. Genzel
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
F. Eisenhauer
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
T. Fritz
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany
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Abstract

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Recently the gas and dust cloud “G2” was discovered on a highly eccentric orbit around the massive black hole in the Galactic center. The orbit will bring the cloud as close as 2400 Schwarzschild radii to Sgr A* beginning of 2014. With the help of hydrodynamical simulations using the PLUTO code, we investigate possible origins and the fate of the cloud in the coming years. In this proceedings article, we concentrate on a scenario where G2 is interpreted as a diffuse gas cloud and show its detailed evolution in the observable position-velocity diagrams. We further elaborate on the problem of the tail emission which might or might not be related to the G2 cloud.

Keywords

black hole physics — hydrodynamics — methods: numerical — ISM: clouds — Galaxy: center
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. 324 - 326
Copyright
Copyright © International Astronomical Union 2014 

References

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