LIU MIT 2006

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Published on November 28, 2007

Author: BAWare

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Electron Acceleration in Magnetized Accretion Disks:  Electron Acceleration in Magnetized Accretion Disks Siming Liu Los Alamos National Laboratory, T-6 Jon Bittner (Yale), Vahé Petrosian (Stanford), Fulvio Melia (U of A), Chris Fryer (LANL) MIT, Oct 20 2006 Outline:  Outline From MHD Simulations to Observations Energy Flow in Black Hole Accretion Electron Acceleration in Magnetized Accretion Disks Testing the Acceleration Model From MHD Simulations to Observations:  From MHD Simulations to Observations MHD Simulation of Accretion Torus in Sgr A*:  MHD Simulation of Accretion Torus in Sgr A* Spectral Methods; Pseudo-Newtonian Potential M = 3.4*106 Msun From 1.5 r_S to 20 r_S; Scale height: H = r_S Chan et al. 2006 QPOs: Accretion Rate:  QPOs: Accretion Rate Chan et al. 2006 QPOs: Light Curve:  QPOs: Light Curve Chan et al. 2006 Emission Model Parameters:  Emission Model Parameters Thermal: Good for thin disk Two Temperature: 1 Plus a power law tail: 4 (Emin, Emax, p, N) Broken power law: 2 Structure of the Accretion Flow:  Structure of the Accretion Flow De Villiers et al. 2003 ApJ Energy Flow in Black Hole Accretion:  Energy Flow in Black Hole Accretion MRI Gravitational Energy  Magnetic Turbulence  Internal Energy + Radiation + Outflow Coupling between Electrons and Protons in Magnetized Disks:  Coupling between Electrons and Protons in Magnetized Disks Magnetic Fields play important roles in electron heating and cooling. It also provides the stress for accretion. If magnetic field pressure is proportional to the stress, the coupling between electrons and protons can be addresses self-consistently. Slide11:  Stochastic Electron Acceleration in Magnetized Accretion Disks Stochastic Electron Acceleration:  Stochastic Electron Acceleration Liu et al. 2006 Evolution of Electron Spectrum:  Evolution of Electron Spectrum Bittner et al. 2006 Evolution of Synchrotron Spectrum:  Evolution of Synchrotron Spectrum Bittner et al. 2006 Stochastic Electron Heating:  Stochastic Electron Heating Bittner et al. 2006 Evolution of Mean Energy:  Evolution of Mean Energy Bittner et al. 2006 a=1.6 a=1.0 Relative Error of the Model:  Relative Error of the Model Bittner et al. 2006 Stochastic Electron Heating:  Stochastic Electron Heating Bittner et al. 2006 Slide19:  Testing the Acceleration Model Thermal Synchrotron:  Thermal Synchrotron Thermal Synchrotron and SSC:  Thermal Synchrotron and SSC Slide22:  Liu et al. 2006 Steady-State Liu et al. 2006 Thermal Synchrotron and SSC:  Thermal Synchrotron and SSC Four Parameters B, kBT = γcmec2, N , A≈R2 Structure of the Accretion Flow:  Structure of the Accretion Flow De Villiers et al. 2003 ApJ Sub-mm Emission from Sgr A*:  Sub-mm Emission from Sgr A* Slide26:  Acceleration within 20rS M87:  M87 Biretta et al. 1999 Flares from Sgr A*:  Flares from Sgr A* Liu et al. 2006 Conclusion:  Conclusion Electron acceleration needs to be addressed to study magnetized accretion disks. In collisionless plasma, magnetic turbulence play roles in electron heating, cooling and driving the accretion. Observations and MHD simulations can test the electron heating model.

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