Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-26T04:53:13.668Z Has data issue: false hasContentIssue false
  • English
  • Français

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 ,
Salomé Dibi ,
Sera Markoff  and
Chris Fragile
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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Keywords

Sgr A*MHDradiation mechanisms: generalplasmasradiative transferdiffusionacceleration of particles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 104 - 105
Copyright
Copyright © International Astronomical Union 2011

References

Anninos, P., Fragile, P. C., & Salmonson, J. D. 2005, ApJ, 635, 723CrossRefGoogle Scholar
Blumenthal, G. R. & Gould, R. J. 1970, Review of Modern Physics, 42, 237CrossRefGoogle Scholar
Esin, A. A., Narayan, R., Ostriker, E., & Yi, I. 1996, ApJ, 465, 312CrossRefGoogle Scholar
Fragile, P. C. & Meier, D. L. 2009, ApJ, 693, 771CrossRefGoogle Scholar
Mahadevan, R., Narayan, R., & Yi, I. 2009, ApJ, 465, 327CrossRefGoogle Scholar
Melia, F. & Falcke, H. 2001, ARAA, 39, 309CrossRefGoogle Scholar
Quataert, E. 2002, ApJ, 575, 855CrossRefGoogle Scholar
Stepney, S. & Guilbert, P. W. 1983, MNRAS, 204, 1269CrossRefGoogle Scholar