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| Paper: |
Solar Astronomy and its Wealth of Data |
| Volume: |
461, Astronomical Data Analysis Software and Systems XXI |
| Page: |
457 |
| Authors: |
Rieutord, M. |
| Abstract: |
The only part of the Sun of which we have a detailed view is its
surface. But this surface is also that of its convection zone which
evolves on shorter and shorter time scales as smaller and smaller length
scales are detected. Monitoring the Sun at a given (visible) wavelength
thus generates a data flow which increases as the cube of the spatial
resolution. A series of images covering the whole visible hemisphere of
the Sun at the resolution of a 50 cm aperture would generate a data flow
rate of 0.8Tb per day. However, knowing its physical state reduces to the
knowledge of eight physical quantities: vx, vy, vz, Bx, By, Bz,
ρ, T (velocity, magnetic, density and temperature fields
respectively). In this work, I give the orders of magnitude of the data
flow rates that should be expected for an ideal monitoring of the Sun. I
also discuss the effects of seeing or the physical constraints that
affect the measurement of quantities like the horizontal component of
the velocity field. Finally, I present the various numerical simulations
data sets that have emerged while investigating the dynamics of the Sun. |
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