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Variable and polarized emission from SgrA*†

Published online by Cambridge University Press:  01 August 2006

A. Eckart ,
R. Schödel ,
L. Meyer ,
C. Straubmeier ,
M. Dovčiak ,
V. Karas ,
M. R. Morris  and
F. K. Baganoff
A. Eckart
Affiliation:
I. Physikalisches Institut, University of Cologne, Zülpicher Str. 77; D-50937 Köln, Germany
R. Schödel
Affiliation:
I. Physikalisches Institut, University of Cologne, Zülpicher Str. 77; D-50937 Köln, Germany
L. Meyer
Affiliation:
I. Physikalisches Institut, University of Cologne, Zülpicher Str. 77; D-50937 Köln, Germany
C. Straubmeier
Affiliation:
I. Physikalisches Institut, University of Cologne, Zülpicher Str. 77; D-50937 Köln, Germany
M. Dovčiak
Affiliation:
Astronomical Institute, Academy of Sciences, Boční II, CZ-14131 Prague, Czech Republic
V. Karas
Affiliation:
Astronomical Institute, Academy of Sciences, Boční II, CZ-14131 Prague, Czech Republic
M. R. Morris
Affiliation:
Department of Physics & Astronomy, UCLA, Los Angeles, CA90095-1547, USA
F. K. Baganoff
Affiliation:
Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139-4307, USA
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Abstract

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The super-massive black hole in the Galactic Center (Sagittarius A*) is one of the most exciting targets in the sky. At a distance of ∼ 8 kpc it is about one hundred times closer than the second nearest nucleus of a similar galaxy, M31, and therefore the closest galactic nucleus that we can study. Here we report on the modeling of polarized near-infrared flare emission from SgrA* using a model in which a hot spot is moving on a relativistic orbit around the massive black hole. We also summarize the results from simultaneous radio/near-infrared/X-ray measurements of flare emission.

Keywords

Galaxy: center – Galaxy: nucleus – accretionaccretion disks – black hole physics – radiation mechanisms: non-thermal – relativity

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