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Astronomical Data Analysis Software and Systems VI

ASP Conference Series, Vol. 125, 1997

Editors: Gareth Hunt and H. E. Payne

**D. Vibert, A. Llebaria, T. Netter, L. Balard, and P. Lamy**

Laboratoire d'Astronomie Spatiale,
BP 8, 13376 Marseille CEDEX 12, France,
E-mail: vibert@astrsp-mrs.fr

The photometric representation of coronal structures is based on a geometrical model of the spatial electron density in the corona and computation of the corresponding scattered light. The purpose is to generate synthetic photometric images which can be compared directly with images of the corona obtained either during eclipses or with space coronagraphs.

Density models for the coronal structures have traditionally
been obtained by inversion of the Thomson scattering integral, assuming
* a priori* shapes of the modeled structures. Later, Bohlin & Garrison
(1974) adopted the direct approach in the form of a
general program based on numerical integration along specified lines
of sight to find the emergent Thomson scattered white light.

Today, the coronal plasma model involves MHD processes. However, numerical physical models of the corona cannot be implemented for high resolution in size and magnitude with classical finite element methods, due to the amount of data one has to cope with. In order to be able to simulate images of the corona at high resolutions we concentrate on the simulation program, improving the methods of Bohlin & Garrison, and incorporating an octree representation of the electron density.

In this paper, we first explain the coronal spatial electron density model and the equations to compute the scattered white light. We then describe the octree representation and coding used, and the algorithms used to integrate along a line of sight through the octree data structure. Finally, we present a sequence of computed images displaying the corona over a solar rotation.

Given the electron density in the coronal plasma, we compute the photospheric light scattered by the coronal electrons:

where is the electron density, **C** is a constant depending upon
electron scattering cross-section and mean solar
brightness, **A** and **B** are two coefficients derived from the
limb-darkening of the Sun and the distance from the electron to the
Sun center, **dz** is a path element along the line-of-sight, and
is the scattering angle-that is, the angle between the
line-of-sight and the line from Sun center to scattering point.

**Figure:**
Sequence of 20 simulated images with the electron density based
upon the neutral sheet for Carrington rotation 1901 (20 Sep-27 Oct 1995). Frame increases first from left to right and
second top to bottom. The time interval between images is one
day. The rapid radial decrease in brightness has been
compensated. Source for the neutral line: Solar Geophysical
Data, no. 617 (January 1996), synoptic chart of the source
surface field on p. 39. Original PostScript figure (2.7MB).

The models attempt to explain the observed coronal streamers as structures associated with the neutral magnetic sheet of the Sun, seen edge-on (Saito et al. 1993).

The corresponding electron density is written as a product of two independent functions:

is the radial decrease along the axis of the streamer and
depends only upon **r**, the distance from the considered point to the
Sun center. This function has been derived from eclipse observations
of streamers. represents the shape of the neutral sheet
and is restricted to a variation with the distance **d** from the
considered point to the neutral sheet. We have chosen for :

a smooth function sharper than a simple Gaussian. The parameter represents half the ``thickness'' of the streamer.

The shape of the neutral sheet is then defined as the radial extension of the neutral line observed on the photosphere, for one Carrington rotation.

An octree is a tree-structured representation that can be used to describe a set of volumetric data enclosed by a bounding cube. The octree is constructed by recursively subdividing each cube into eight sub-cubes, starting at a single large cube represented by the root-node in the tree. A cube will have descendants only if its associated volume of object space is not homogeneous. The recursion continues until either all sub-cubes are homogeneous or until the required resolution is achieved.

A number of efficient schemes have been developed to represent and
encode octrees. The **S**-tree type (Jonge, Scheuermann, & Schijf 1994)
linear encoding was implemented in this work. The tree is built
directly from the continuous expression of the coronal electron
density given by the mathematical expressions (Eq. 76).
The subdivision criterion for a cube is the variation of the
electron density within the cube.

The traversal of the octree data structure to determine the leafs hit by a line-of-sight relies on the HERO algorithm (Agate, Grimsdale, & Lister 1991). At each level of the octree, the algorithm generates the addresses of child voxels (volume elements) in the order they are penetrated by the ray, avoiding the time consuming test of determining the intersection between the ray and the eight children for every node in the tree.

Such octree coding and ray-tracing methods lead to significant
improvements in terms of resolution, compression, and speed. The
generation of an octree of size **1024 × 1024 × 1024**, based on smallest
voxel size, with 4 byte floating point values, takes approximately two hours
(using a standard low cost workstation with 64MB of memory) and
requires 60MB of disk space. The same data uniformly sampled at the
same resolution would have required 4096MB.

The ray-trace reconstruction of the former octree-based data produces
white light images with a resolution of **512 × 512** pixels, in less
than half an hour. A uniform sampling (e.g., by 1024) of every
line-of-sight (every pixel) would have led to a far longer computing
time for the same output.

This relatively short time necessary to compute one image allows to compute a temporal sequence of images showing corona aspect variations with Sun rotation (Figure 1).

Agate, M., Grimsdale, R. L., & Lister P. F. 1991, in Advances in Computer Graphics Hardware IV, ed. R. L. Grimsdale & W. Strasser (Dordrecht: Springer-Verlag), 61

Bohlin, J. D., & Garrison, L. M. 1974, Solar Physics, 38, 271

de Jonge, W. P., Scheuermann, P., & Schijf, A. 1994, Comput. Vision Graphics and Image Processing, 24, 1

Saito, T., Akasofu, S. I., Takahashi, Y., & Numazawa, S. 1993, Journal of Geophysical Research, 98, 5639

© Copyright 1997 Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, California 94112, USA

** Next:** Error and Bias in the STSDAS fitting Package

** Previous:** Using Massively Parallel Processing of a NLTE Spectrum Synthetic Code and an Automated Comparison with Observations to Determine the Properties of Type Ia Supernovae from their Late Time Spectra.

**Up:** Modeling

Table of Contents - Index - PS reprint

payne@stsci.edu