Advances in Modeling the initiation and evolution of CMEs through the Solar WInd

Details Advances in Modeling the initiation and evolution of CMEs through the Solar WInd Advances in Modeling the initiation and evolution of CMEs through the Solar WInd

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh53c..05r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH53C-05

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections

Scientific paper

Over the last decade, several factors have led to remarkable gains in our ability to realistically model a coronal mass ejection (CME) all the way from the solar surface to 1 AU, or beyond. First, global models of the ambient solar corona and inner heliosphere have improved dramatically. The algorithms have transitioned from simple polytropic prescriptions to rich thermodynamic models that can reproduce the essential features of remote solar observations and in-situ measurements. Second, theories of CME initiation, and their implementation into numerical models, have developed to the point that a range of complex mechanisms can now be simulated with great fidelity. Third, the original serial codes are now fully parallelized allowing them to recruit thousands of processors, and with this, the ability to simulate events on unprecedented temporal and spatial scales. And fourth, successive NASA-led missions are returning ever-more resolved and accurate photospheric magnetic field observations from which boundary conditions can be derived. In this talk, we show how these factors have allowed us to produce event-specific simulations that provide genuine insight into the initiation and evolution of CMEs, and contrast these results with what was "state-of-the-art" only 10 years ago. We close by speculating on what the next advances in global CME models might be.

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