Magnetized (“ real ”) Accretion Flows Roman Shcherbakov, 5 December, 2007.

Slides:

Advertisements

Similar presentations

Experimental tasks Spectra Extend to small scale; wavenumber dependence (Taylor hyp.); density, flow Verify existence of inertial range Determine if decorrelation.

Advertisements

Turbulent transport of magnetic fields Fausto Cattaneo Center for Magnetic Self-Organization in Laboratory and Astrophysical.

Progress and Plans on Magnetic Reconnection for CMSO For NSF Site-Visit for CMSO May1-2, Experimental progress [M. Yamada] -Findings on two-fluid.

Outline: I. Introduction and examples of momentum transport II. Momentum transport physics topics being addressed by CMSO III. Selected highlights and.

The Accretion of Poloidal Flux by Accretion Disks Princeton 2005.

Magnetic Chaos and Transport Paul Terry and Leonid Malyshkin, group leaders with active participation from MST group, Chicago group, MRX, Wisconsin astrophysics.

Global Simulations of Astrophysical Jets in Poynting Flux Dominated Regime Hui Li S. Colgate, J. Finn, G. Lapenta, S. Li Engine; Injection; Collimation;

General Meeting Madison, August 4-6, 2004 Plans and Progress of Magnetic Helicity Conservation and Transport H. Ji for participants of the Center for Magnetic.

Simulating the Extreme Environment Near Luminous Black Hole Sources Omer Blaes University of California, Santa Barbara.

“The interaction of a giant planet with a disc with MHD turbulence I: The initial turbulent disc models” Papaloizou & Nelson 2003a, MNRAS 339, 923 Brian.

Processes in Protoplanetary Disks Phil Armitage Colorado.

粒子シミュレーションで観る粒子加速 : 衝撃波、リコネクション、降着円盤星野真弘. Nonthermal Universe Cosmic Rays ACRs [Stone et al., 2008] Where and How are non-thermal particles produced?

“The interaction of a giant planet with a disc with MHD turbulence II: The interaction of the planet with the disc” Papaloizou & Nelson 2003, MNRAS 339.

Session: MGAT9 – Self-Gravitating Systems SPHERICALLY SYMMETRIC RELATIVISTIC STELLAR CLUSTERS WITH ANISOTROPIC MOMENTUM DISTRIBUTION Marco MERAFINA Department.

Steady Models of Black Hole Accretion Disks including Azimuthal Magnetic Fields Hiroshi Oda (Chiba Univ.) Mami Machida (NAOJ) Kenji Nakamura (Matsue) Ryoji.

SELF-SIMILAR SOLUTIONS OF VISCOUS RESISTIVE ACCRETION FLOWS Jamshid Ghanbari Department of Physics, School of Sciences, Ferdowsi University of Mashhad,

Muduleya LEI 1 Modeling the Accretion Flow Around the SMBH at the Galactic Center Lei Huang Center for Astrophysics, USTC Collaborators:

Numerical simulations of the magnetorotational instability (MRI) S.Fromang CEA Saclay, France J.Papaloizou (DAMTP, Cambridge, UK) G.Lesur (DAMTP, Cambridge,

General Relativistic MHD Simulations of Black Hole Accretion Disks John F. Hawley University of Virginia Presented at the conference on Ultra-relativistic.

GENERAL RELATIVISTIC MHD SIMULATIONS OF BLACK HOLE ACCRETION with: Kris Beckwith, Jean-Pierre De Villiers, John Hawley, Shigenobu Hirose, Scott Noble,

Theoretical Calculations of the Inner Disk’s Luminosity Scott C. Noble, Julian H. Krolik (JHU) (John F. Hawley, Charles F. Gammie) 37 th COSPAR 2008, E17.

Numerical simulations of the MRI: the effects of dissipation coefficients S.Fromang CEA Saclay, France J.Papaloizou (DAMTP, Cambridge, UK) G.Lesur (DAMTP,

Models of Turbulent Angular Momentum Transport Beyond the  Parameterization Martin Pessah Institute for Advanced Study Workshop on Saturation and Transport.

On Forming a Jet inside the magnetized envelope collapsing onto a black hole D. Proga.

ADIOS Revisited Mitch Begelman JILA, University of Colorado ADIOS Revis it ed.

Processes in Protoplanetary Disks

A Critical Role for Viscosity in the Radio Mode AGN Feedback Cycle Paul Nulsen Harvard-Smithsonian Center for Astrophysics 2014 July 9X-ray View of Galaxy.

1 Hantao Ji Princeton Plasma Physics Laboratory Experimentalist Laboratory astrophysics –Reconnection, angular momentum transport, dynamo effect… –Center.

The Air-Sea Momentum Exchange R.W. Stewart; 1973 Dahai Jeong - AMP.

Type I Migration with Stochastic Torques Fred C. Adams & Anthony M. Bloch University of Michigan Fred C. Adams & Anthony M. Bloch University of Michigan.

Processes in Protoplanetary Disks Phil Armitage Colorado.

Kinetic Effects on the Linear and Nonlinear Stability Properties of Field- Reversed Configurations E. V. Belova PPPL 2003 APS DPP Meeting, October 2003.

Shocks! David Burgess Astronomy Unit Queen Mary, University of London.

Radiation Hydrodynamic simulations of super-Eddington Accretion Flows super-Eddington Accretion Flows Radiation Hydrodynamic simulations of super-Eddington.

Semi-Empirical MHD Modeling of the Solar Wind Igor V. Sokolov, Ofer Cohen, Tamas I. Gombosi CSEM, University of Michigan Ilia I Roussev, Institute for.

Boundaries, shocks, and discontinuities. How discontinuities form Often due to “wave steepening” Example in ordinary fluid: –V s 2 = dP/d  m –P/  

Magnetic Fields and Jet Formation John F. Hawley University of Virginia Workshop on MRI Turbulence June 18 th 2008.

Radiatively Inefficient Accretion Flows Roman Shcherbakov, 28 November, 2007.

Large scale magnetic fields and Dynamo theory Roman Shcherbakov, Turbulence Discussion Group 14 Apr 2008.

Three-dimensional MHD Simulations of Jets from Accretion Disks Hiromitsu Kigure & Kazunari Shibata ApJ in press (astro-ph/ ) Magnetohydrodynamic.

Angular momentum conservation: 1

MHD JET ACCELERATION AMR SIMULATIONS Claudio Zanni, Attilio Ferrari, Silvano Massaglia Università di Torino in collaboration with Gianluigi Bodo, Paola.

Stability Properties of Field-Reversed Configurations (FRC) E. V. Belova PPPL 2003 International Sherwood Fusion Theory Conference Corpus Christi, TX,

BGU WISAP Spectral and Algebraic Instabilities in Thin Keplerian Disks: I – Linear Theory Edward Liverts Michael Mond Yuri Shtemler.

Magnetic activity in protoplanetary discs Mark Wardle Macquarie University Sydney, Australia Catherine Braiding (Macquarie) Arieh Königl (Chicago) BP Pandey.

Variability of radio-quiet AGN across the spectrum: facts and ideas B. Czerny Copernicus Astronomical Center, Warsaw, Poland.

Magnetohydrodynamic simulations of stellar differential rotation and meridional circulation (submitted to A&A, arXiv: ) Bidya Binay Karak (Nordita.

The Magneto-Rotational Instability and turbulent angular momentum transport Fausto Cattaneo Paul Fischer Aleksandr Obabko.

The Magnetorotational Instability

June 08MRI Transport properties1 MRI-driven turbulent resistivity Pierre-Yves Longaretti (LAOG) Geoffroy Lesur (DAMTP)

Stability of Expanding Jets Serguei Komissarov & Oliver Porth University of Leeds and Purdue University TexPoint fonts used in EMF. Read the TexPoint manual.

11/01/2016 Variable Galactic Gamma-Ray Sources, Heidelberg, Germany 1 Maxim Barkov MPI-K, Heidelberg, Germany Space Research Institute, Russia, University.

Reynolds Analogy It can be shown that, under specific conditions (no external pressure gradient and Prandtle number equals to one), the momentum and heat.

General Relativistic MHD Simulations of Black Hole Accretion Disks John F. Hawley University of Virginia Presented at the Astrophysical Fluid Dynamics.

Black Hole Accretion, Conduction and Outflows Kristen Menou (Columbia University) In collaboration with Taka Tanaka (GS)

Lecture 3. Full statistical description of the system of N particles is given by the many particle distribution function: in the phase space of 6N dimensions.

Magnetorotational Instability (MRI) Experiment

Brookhaven Science Associates U.S. Department of Energy MERIT Project Review December 12, 2005, BNL, Upton NY MHD Studies of Mercury Jet Target Roman Samulyak.

Gamma-Ray Bursts and unmagnetized relativistic collisionless shocks Ehud Nakar Caltech.

Global 3D MHD Simulations of Optically Thin Black Hole Accretion Disks

MHD and Kinetics Workshop February 2008 Magnetic reconnection in solar theory: MHD vs Kinetics Philippa Browning, Jodrell Bank Centre for Astrophysics,

Disk Dynamics Julian Krolik Johns Hopkins University.

GR/MHD SIMULATIONS OF JET-LAUNCHING Collaborators: J.P. De Villiers, J.F. Hawley, S. Hirose.

GR/MHD SIMULATIONS OF ACCRETION ONTO BLACK HOLES (cont.) Jean-Pierre De Villiers John Hawley Shigenobu Hirose JHK.

ANGULAR MOMENTUM TRANSPORT BY MAGNETOHYDRODYNAMIC TURBULENCE Gordon Ogilvie University of Cambridge TACHOCLINE DYNAMICS

Mixing Length of Hydrogen in an Air Intake Greg Lilik EGEE 520.

GEM Student Tutorial: GGCM Modeling (MHD Backbone)

Plasma outflow from dissipationless accretion disks

Dynamo action & MHD turbulence (in the ISM, hopefully…)

Contents Introduction Force-Free Approximation Analytical Solutions

Presentation transcript:

Magnetized (“ real ”) Accretion Flows Roman Shcherbakov, 5 December, 2007

Specifics of Magnetized accretion Coulomb mean free path > size of the flow Proton gyroradius < size of the flow collisionless MHD (not full kinetic theory) collisionless MHD Plasma beta parameterMagnetization in the real flows, thus magnetic field is usually dynamically important

Spherical accretion. Problem

Spherical accretion. Setup Outer magnetization radius of influence of BH/NS – Compression maintains turbulence Balance between build-up and dissipation Externally supported Isotropic turbulence Supported by compression Non-Isotropic turbulence

Spherical accretion. Accretion rate Relativistic EOS Larger inhibition Larger magnetizaton Smaller accretion rate outer magnetization normalized accretion rate Larger back-reaction

Spherical accretion. Magnetization

Magnetorotational Instability

Evolution of MRI z

Transport of angular momentum Reynolds stress (>0) Maxwell stress (<0) Schwarz inequality Also Upper boundary for stress stress is important, angular momentum can go up and be carried away by wind

vs Kato, Yoshizawa, 1995PASJ K turbulent stress coefficient energy generation coefficient

Evolution of magnetization

Evolution of angular momentum alpha

Density contours CK Chan, 2007

Analytic closures Pessah, CK Chan 2007

Krolik, 2005

Hawley, Balbus 2002

Conclusions Magnetic field is an essential ingredient of ANY astrophysical flow Realistic accretion pattern is likely to be very complicated, outflows, jets Alpha parameter should at least be a function of radius, but apparently one parameter is not enough Zero torque condition at ISCO is not applicable Some analytic calculations, but progress is made through simulations