The Nature of Linearly Polarized Millimeter and Sub-millimeter Emission in Sagittarius A*
arXiv:0705.2792 · doi:10.1086/522832
Abstract
The linearly polarized millimeter and sub-millimeter emission in Sagittarius A* is produced within 10 Schwarzschild radii of the supermassive black hole at the Galactic Center and may originate from a hot magnetized accretion disk, where electrons are heated efficiently by turbulent plasma waves. In such a scenario, the flux density and polarization are very sensitive to the electron heating rate and the inclination angle of disk, respectively, and the major axis of the sub-millimeter intrinsic polarization, which is aligned with the rotation axis of the disk, is perpendicular to the major axis of the polarized near-infrared emission. In combination with MHD simulations, which study the properties of the magnetic field and viscous stresses, the current spectral and polarization measurements give tight constraints on the model parameters. Simultaneous observations will be able to test the model.
With the new version accepted by ApJ Letter
References in corpus (10)
- An Unambiguous Detection of Faraday Rotation in Sagittarius A*
- Polarimetry of near-infrared flares from Sagittarius A*
- Flaring Activity of Sgr A* at 43 and 22 GHz: Evidence for Expanding Hot Plasma
- A Constant Spectral Index for Sagittarius A* During Infrared/X-ray Intensity Variations
- The Rotation Measure and 3.5mm Polarization of Sgr A*
- K-band polarimetry of an Sgr A* flare with a clear sub-flare structure
- Black Hole Shadow Image and Visibility Analysis of Sagittarius A*
- The Submillimeter Polarization of Sgr A*
- A Local Model for Angular Momentum Transport in Accretion Disks Driven by the Magnetorotational Instability
- A Testable the Stochastic Acceleration Model for Flares in Sagittarius A*