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Self-consistent spectra from GRMHD simulations with radiative cooling A link to reality for Sgr A*

Published online by Cambridge University Press:  24 February 2011

Samia Drappeau
Affiliation:
Sterrenkundig Instituut ‘Anton Pannekoek’, Universiteit van Amsterdam, Postbus 94249, 1090GE Amsterdam, the Netherlands email: s.drappeau@uva.nl, s.dibi-rousselle@uva.nl, s.markoff@uva.nl
Salomé Dibi
Affiliation:
Sterrenkundig Instituut ‘Anton Pannekoek’, Universiteit van Amsterdam, Postbus 94249, 1090GE Amsterdam, the Netherlands email: s.drappeau@uva.nl, s.dibi-rousselle@uva.nl, s.markoff@uva.nl
Sera Markoff
Affiliation:
Sterrenkundig Instituut ‘Anton Pannekoek’, Universiteit van Amsterdam, Postbus 94249, 1090GE Amsterdam, the Netherlands email: s.drappeau@uva.nl, s.dibi-rousselle@uva.nl, s.markoff@uva.nl
Chris Fragile
Affiliation:
Dept. of Physics & Astronomy, College of Charleston, Charleston, USA email: fragilep@cofc.edu
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Abstract

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Cosmos++ (Anninos et al. 2005) is one of the first fully relativistic magneto-hydro-dynamical (MHD) codes that can self-consistently account for radiative cooling, in the optically thin regime. As the code combines a total energy conservation formulation with a radiative cooling function, we have now the possibility to produce spectra energy density from these simulations and compare them to data. In this paper, we present preliminary results of spectra calculated using the same cooling functions from 2D Cosmos++ simulations of the accretion flow around Sgr A*. The simulation parameters were designed to roughly reproduce Sgr A*'s behavior at very low (10−8–10−7 M/yr) accretion rate, but only via spectra can we test that this has been achieved.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

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