The central cluster and X-ray emission from Sgr A*

Details The central cluster and X-ray emission from Sgr A* The central cluster and X-ray emission from Sgr A*

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..347c&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Computer Science

Scientific paper

At the centre of the Milky Way is Sgr A*, a putative 3 million solar mass black hole with an observed luminosity that is orders of magnitude smaller than that expected from simple accretion theories. The number density of early-type stars is quite high near Sgr A*, so the ensemble of their stellar winds has a significant impact on the black hole's environment and diet. We present results of 3D hydrodynamic simulations of the accretion of stellar winds onto Sgr A*. Using the LANL/SAIC code, RAGE, we model the central arc-second of the Galaxy, including the central cluster stars (the `S' stars) with orbits and wind parameters that match observations. We include optically thin radiative cooling and the gravitational potential of the black hole and the underlying stellar cluster. A significant fraction of the winds from the `S' stars becomes gravitationally bound to the black hole and thus could provide enough hot gas to produce the X-ray emission seen by Chandra. We perform radiative transfer calculations on the 3D hydrodynamic data cubes, producing synthetic X-ray images and spectra to compare to the Chandra data. We present these results and discuss the implications for Sgr A* accretion models.

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