MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric Model.
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Transcript of MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric Model.
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MHD Modeling of the Large Scale Solar Corona & Progress Toward Coupling with the Heliospheric
Model
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Goals• To model physical processes from above
the transition region to the inner heliosphere (approximately 1 – 20 RS).
• The model will provide density, temperature, plasma velocity and magnetic field within this region.
• Couple the model to ENLIL (Dusan’s heliosphere code) in order to drive solar wind conditions at 1 AU.
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Ultimate Goal of the Coronal MHD Modeling
• To input a synoptic map (Magnetic field in the photosphere) into the model and get out realistic coronal and solar wind parameters– Density
– Temperature
– Velocity
– Magnetic field structure
• Note this included active region scales and their effects on the global scale.
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The Physical Process in the Corona are not well understood
• Heating Processes– What heats the coronal plasma? – How is the heating distributed?
• Wind Acceleration– How is the high speed solar wind accelerated.
• The lower boundary conditions are not well defined. – The same boundary issues that occur when
modeling a active region applies here.
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McComas et al., 1998
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Tools
• Static mesh MHD model (modified version of Zeus-3D) for testing and development.
• A Spherically Adaptive Mesh MHD model (ZeusAMR) for the global simulations.
• 3D MHD model (Enlil) for global heliospheric simulations (up to 5 AU).
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Tool Status
• Static Mesh Model– Runs relatively quickly (depending on res.)– Includes Alfvén wave wind acceleration and
heating.– Work in progress includes:
• Adding or trying to parameterize radiative losses, collisionless and Spitzer conductivities.
• Incorporating synoptic maps to provide lower boundary conditions on the magnetic field.
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Alfvén Wave Driven Wind Speeds in a Dipole Field Configuration
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Spherical ZeusAMR Model
• Under development.• Currently working axisymmetric wedge
shaped domains (Cartesian version of ZeusAMR is working).
• Parallelization is underway.• The groundwork needed to couple the
model to the ENLIL heliosphere model has been incorporated.
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Including Active Region Effects in the Global Corona. ZeusAMR Coronal model, initialized with PFSS model of CR1918.
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Synthetic White-Light Imaging
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Conclusions
• Development of the Coronal MHD model is well underway.
• We plan to have a coupled Coronal-Heliospheric MHD simulation by early summer.
• Future plans include coupling the global coronal model to data driven MHD models of active regions (Abbett).