GRAND MINIMA AND EQUATORWARD PROPAGATION IN A CYCLING STELLAR CONVECTIVE DYNAMO
Abstract
The 3D MHD Anelastic Spherical Harmonic code, using slopelimited diffusion, is employed to capture convective and dynamo processes achieved in a globalscale stellar convection simulation for a model solarmass star rotating at three times the solar rate. The dynamogenerated magnetic fields possesses many timescales, with a prominent polarity cycle occurring roughly every 6.2 years. The magnetic field forms largescale toroidal wreaths, whose formation is tied to the low Rossby number of the convection in this simulation. The polarity reversals are linked to the weakened differential rotation and a resistive collapse of the largescale magnetic field. An equatorial migration of the magnetic field is seen, which is due to the strong modulation of the differential rotation rather than a dynamo wave. A poleward migration of magnetic flux from the equator eventually leads to the reversal of the polarity of the highlatitude magnetic field. This simulation also enters an interval with reduced magnetic energy at low latitudes lasting roughly 16 years (about 2.5 polarity cycles), during which the polarity cycles are disrupted and after which the dynamo recovers its regular polarity cycles. An analysis of this grand minimum reveals that it likely arises through the interplay of symmetric and antisymmetric dynamo families.more »
 Authors:
 High Altitude Observatory, Center Green 1, Boulder, CO 80301 (United States)
 Laboratoire AIM ParisSaclay, CEA/DSM–CNRS–Université Paris Diderot, IRFU/SAp, GifsurYvette (France)
 JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States)
 Publication Date:
 OSTI Identifier:
 22525557
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: Astrophysical Journal; Journal Volume: 809; 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; COMPUTERIZED SIMULATION; CONVECTION; DIFFUSION; MAGNETIC FIELDS; MAGNETIC FLUX; MAGNETOHYDRODYNAMICS; MAIN SEQUENCE STARS; MEANFIELD THEORY; MODULATION; PRANDTL NUMBER; ROTATION; SPHERICAL CONFIGURATION; STAR MODELS; TURBULENCE
Citation Formats
Augustson, Kyle, Miesch, Mark, Brun, Allan Sacha, and Toomre, Juri. GRAND MINIMA AND EQUATORWARD PROPAGATION IN A CYCLING STELLAR CONVECTIVE DYNAMO. United States: N. p., 2015.
Web. doi:10.1088/0004637X/809/2/149.
Augustson, Kyle, Miesch, Mark, Brun, Allan Sacha, & Toomre, Juri. GRAND MINIMA AND EQUATORWARD PROPAGATION IN A CYCLING STELLAR CONVECTIVE DYNAMO. United States. doi:10.1088/0004637X/809/2/149.
Augustson, Kyle, Miesch, Mark, Brun, Allan Sacha, and Toomre, Juri. 2015.
"GRAND MINIMA AND EQUATORWARD PROPAGATION IN A CYCLING STELLAR CONVECTIVE DYNAMO". United States.
doi:10.1088/0004637X/809/2/149.
@article{osti_22525557,
title = {GRAND MINIMA AND EQUATORWARD PROPAGATION IN A CYCLING STELLAR CONVECTIVE DYNAMO},
author = {Augustson, Kyle and Miesch, Mark and Brun, Allan Sacha and Toomre, Juri},
abstractNote = {The 3D MHD Anelastic Spherical Harmonic code, using slopelimited diffusion, is employed to capture convective and dynamo processes achieved in a globalscale stellar convection simulation for a model solarmass star rotating at three times the solar rate. The dynamogenerated magnetic fields possesses many timescales, with a prominent polarity cycle occurring roughly every 6.2 years. The magnetic field forms largescale toroidal wreaths, whose formation is tied to the low Rossby number of the convection in this simulation. The polarity reversals are linked to the weakened differential rotation and a resistive collapse of the largescale magnetic field. An equatorial migration of the magnetic field is seen, which is due to the strong modulation of the differential rotation rather than a dynamo wave. A poleward migration of magnetic flux from the equator eventually leads to the reversal of the polarity of the highlatitude magnetic field. This simulation also enters an interval with reduced magnetic energy at low latitudes lasting roughly 16 years (about 2.5 polarity cycles), during which the polarity cycles are disrupted and after which the dynamo recovers its regular polarity cycles. An analysis of this grand minimum reveals that it likely arises through the interplay of symmetric and antisymmetric dynamo families. This intermittent dynamo state potentially results from the simulation’s relatively low magnetic Prandtl number. A meanfieldbased analysis of this dynamo simulation demonstrates that it is of the αΩ type. The timescales that appear to be relevant to the magnetic polarity reversal are also identified.},
doi = {10.1088/0004637X/809/2/149},
journal = {Astrophysical Journal},
number = 2,
volume = 809,
place = {United States},
year = 2015,
month = 8
}

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