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arXiv · 1609.07318

3D AMR simulations of G2 as an outflow

A. Ballone·M. Schartmann·A. Burkert·S. Gillessen·P. M. Plewa·O. Pfuhl·R. Genzel·F. Eisenhauer·T. Ott·E. M. George·M. Habibi
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Abstract

We study the evolution of G2 in a \textit{Compact Source Scenario}, where G2 is the outflow from a low-mass central star moving on the observed orbit. This is done through 3D AMR simulations of the hydrodynamic interaction of G2 with the surrounding hot accretion flow. A comparison with observations is done by means of mock position-velocity (PV) diagrams. We found that a massive ($\dot{M}_\mathrm{w}=5\times 10^{-7} \;M_{\odot} \; \mathrm{yr^{-1}}$) and slow ($v_\mathrm{w}=50 \;\mathrm{km\; s^{-1}}$) outflow can reproduce G2's properties. A faster outflow ($v_\mathrm{w}=400 \;\mathrm{km\; s^{-1}}$) might also be able to explain the material that seems to follow G2 on the same orbit.

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A. Ballone, M. Schartmann, A. Burkert, S. Gillessen, P. M. Plewa, O. Pfuhl, R. Genzel, F. Eisenhauer, T. Ott, E. M. George, M. Habibi. 2016-09-23. 3D AMR simulations of G2 as an outflow. https://doi.org/10.1017/s1743921316012345

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