3D adaptive mesh refinement simulations of the gas cloud G2 born within
  the disks of young stars in the Galactic Center
  The dusty, ionized gas cloud G2 is currently passing the massive black hole
in the Galactic Center at a distance of roughly 2400 Schwarzschild radii. We
explore the possibility of a starting point of the cloud within the disks of
young stars. We make use of the large amount of new observations in order to
put constraints on G2's origin. Interpreting the observations as a diffuse
cloud of gas, we employ three-dimensional hydrodynamical adaptive mesh
refinement (AMR) simulations with the PLUTO code and do a detailed comparison
with observational data. The simulations presented in this work update our
previously obtained results in multiple ways: (1) high resolution
three-dimensional hydrodynamical AMR simulations are used, (2) the cloud
follows the updated orbit based on the Brackett-$\gamma$ data, (3) a detailed
comparison to the observed high-quality position-velocity diagrams and the
evolution of the total Brackett-$\gamma$ luminosity is done. We concentrate on
two unsolved problems of the diffuse cloud scenario: the unphysical formation
epoch only shortly before the first detection and the too steep
Brackett-$\gamma$ light curve obtained in simulations, whereas the observations
indicate a constant Brackett-$\gamma$ luminosity between 2004 and 2013. For a
given atmosphere and cloud mass, we find a consistent model that can explain
both, the observed Brackett-$\gamma$ light curve and the position-velocity
diagrams of all epochs. Assuming initial pressure equilibrium with the
atmosphere, this can be reached for a starting date earlier than roughly 1900,
which is close to apo-center and well within the disks of young stars.
