The Nature of Linearly Polarized Millimeter and Sub-millimeter Emission in Sagittarius A*

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.

arXiv commentWith the new version accepted by ApJ Letter

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Cited by in corpus (6)

• Testing the Accretion Flow with Plasma Wave Heating Mechanism for Sagittarius a* by the 1.3MM Vlbi Measurements
• Linearly Polarized Millimeter and Submillimeter Continuum Emission of Sgr A* Constrained by ALMA
• Polarized Emission of Sagittarius A*
• The 492 GHz emission of Sgr A* constrained by ALMA
• Near-infrared Polarimetry of flares from Sgr A* with Subaru/CIAO
• Impact of the nonthermal electron radiation effects on the horizon scale image structure of Sagittarius A*