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Additional info for ACM Transactions on Graphics (January)

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In spite of that, we believe that a more natural way to model plasma phenomena is to simulate the equations of plasma flow directly. The use of a plasma model allows the control of the simulations by auroral physically meaningful parameters. Moreover, the use of a plasma model enables the accurate reproduction of the rapid intermediate scale motions often seen in the aurorae such as the motion of rays and folds along auroral forms. Recent works on night sky phenomena have focused on obtaining images that are not only realistic, but are also predictive.

Rapidly. These complex and stochastic motions are directly related to the plasma processes. In this article, a novel physically-based model to perform 3D visual simulations of the dynamics of the auroral phenomena is presented. Furthermore, auroral surges (Figure 14), which have not been previously simulated, are also rendered. This model, therefore, enables the simulation of shape and motion of the aurorae in a realistic manner. The aurorae are frequently visible at high latitudes. They can also be seen less frequently at lower latitudes, especially around solar sunspot maxima (a period of great solar turbulence that occurs approximately every 11 years [Odenwald 2000]).

Rendering issues are further examined in Section 5. ACM Transactions on Graphics, Vol. 24, No. 1, January 2005. Simulating the Dynamics of Auroral Phenomena • 45 The auroral dynamics simulation uses the auroral local coordinate system defined in Section 2. The mapping of auroral emissions for rendering purposes uses a global coordinate system represented by XYZ, where the Y-axis corresponds to the direction normal to the ground. 4. DYNAMICS SIMULATION The electron beams interact with one another through the electric field, E, generated by their mutual electrostatic repulsion, and the Earth’s magnetic field, B.

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ACM Transactions on Graphics (January) by Association for Computing Machinery


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