LARGESCALE AZIMUTHAL STRUCTURES OF TURBULENCE IN ACCRETION DISKS: DYNAMO TRIGGERED VARIABILITY OF ACCRETION
Abstract
We investigate the significance of largescale azimuthal, magnetic, and velocity modes for the magnetorotational instability (MRI) turbulence in accretion disks. We perform threedimensional global ideal MHD simulations of global stratified protoplanetary disk models. Our domains span azimuthal angles of {pi}/4, {pi}/2, {pi}, and 2{pi}. We observe up to 100% stronger magnetic fields and stronger turbulence for the restricted azimuthal domain models {pi}/2 and {pi}/4 compared to the full 2{pi} model. We show that for those models the Maxwell stress is larger due to strong axisymmetric magnetic fields generated by the {alpha}{Omega} dynamo. Large radial extended axisymmetric toroidal fields trigger temporal magnification of accretion stress. All models display a positive dynamo{alpha} in the northern hemisphere (upper disk). The parity is distinct in each model and changes on timescales of 40 local orbits. In model 2{pi}, the toroidal field is mostly antisymmetric with respect to the midplane. The eddies of the MRI turbulence are highly anisotropic. The major wavelengths of the turbulent velocity and magnetic fields are between one and two disk scale heights. At the midplane, we find magnetic tilt angles around 8 DegreeSign 9 DegreeSign increasing up to 12 DegreeSign 13 DegreeSign in the corona. We conclude that an azimuthalmore »
 Authors:
 Max Planck Institute for Astronomy, Koenigstuhl 17, 69117 Heidelberg (Germany)
 Publication Date:
 OSTI Identifier:
 22004198
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: Astrophysical Journal; Journal Volume: 744; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; ASTROPHYSICS; AXIAL SYMMETRY; COMPUTERIZED SIMULATION; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; NORTHERN HEMISPHERE; ORBITS; PROTOPLANETS; THREEDIMENSIONAL CALCULATIONS; TURBULENCE
Citation Formats
Flock, M., Dzyurkevich, N., Klahr, H., Turner, N., and Henning, Th. LARGESCALE AZIMUTHAL STRUCTURES OF TURBULENCE IN ACCRETION DISKS: DYNAMO TRIGGERED VARIABILITY OF ACCRETION. United States: N. p., 2012.
Web. doi:10.1088/0004637X/744/2/144.
Flock, M., Dzyurkevich, N., Klahr, H., Turner, N., & Henning, Th. LARGESCALE AZIMUTHAL STRUCTURES OF TURBULENCE IN ACCRETION DISKS: DYNAMO TRIGGERED VARIABILITY OF ACCRETION. United States. doi:10.1088/0004637X/744/2/144.
Flock, M., Dzyurkevich, N., Klahr, H., Turner, N., and Henning, Th. 2012.
"LARGESCALE AZIMUTHAL STRUCTURES OF TURBULENCE IN ACCRETION DISKS: DYNAMO TRIGGERED VARIABILITY OF ACCRETION". United States.
doi:10.1088/0004637X/744/2/144.
@article{osti_22004198,
title = {LARGESCALE AZIMUTHAL STRUCTURES OF TURBULENCE IN ACCRETION DISKS: DYNAMO TRIGGERED VARIABILITY OF ACCRETION},
author = {Flock, M. and Dzyurkevich, N. and Klahr, H. and Turner, N. and Henning, Th.},
abstractNote = {We investigate the significance of largescale azimuthal, magnetic, and velocity modes for the magnetorotational instability (MRI) turbulence in accretion disks. We perform threedimensional global ideal MHD simulations of global stratified protoplanetary disk models. Our domains span azimuthal angles of {pi}/4, {pi}/2, {pi}, and 2{pi}. We observe up to 100% stronger magnetic fields and stronger turbulence for the restricted azimuthal domain models {pi}/2 and {pi}/4 compared to the full 2{pi} model. We show that for those models the Maxwell stress is larger due to strong axisymmetric magnetic fields generated by the {alpha}{Omega} dynamo. Large radial extended axisymmetric toroidal fields trigger temporal magnification of accretion stress. All models display a positive dynamo{alpha} in the northern hemisphere (upper disk). The parity is distinct in each model and changes on timescales of 40 local orbits. In model 2{pi}, the toroidal field is mostly antisymmetric with respect to the midplane. The eddies of the MRI turbulence are highly anisotropic. The major wavelengths of the turbulent velocity and magnetic fields are between one and two disk scale heights. At the midplane, we find magnetic tilt angles around 8 DegreeSign 9 DegreeSign increasing up to 12 DegreeSign 13 DegreeSign in the corona. We conclude that an azimuthal extent of {pi} is sufficient to reproduce most turbulent properties in threedimensional global stratified simulations of magnetized accretion disks.},
doi = {10.1088/0004637X/744/2/144},
journal = {Astrophysical Journal},
number = 2,
volume = 744,
place = {United States},
year = 2012,
month = 1
}

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