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# Turbulence in the Atmosphere

In ground based telescopes, this diffraction-limited resolution is never reached. Ground-based telescopes must look through miles of the Earth's atmosphere. Turbulent fluctuations in the wind velocities in the upper atmosphere mix layers of differing temperatures, densities and water vapor content. Thus the index of refraction of each level of the atmosphere fluctuates. The wavefront incident on the telescope has spatial and temporal variations in phase and amplitude due to these fluctuations in the index of refraction along the optical path. Across the diameter of large telescopes (4 to 8 meters), phase errors are a few m and dominate the degradation of spatial resolution. The spatial resolution of the telescope is degraded to an order of magnitude greater than the diffraction limit and the central intensity of a point source image is degraded by two orders of magnitude. (Hubin & Noethe, 1993).

Turbulence is a non-linear process, and so the equations governing it are non-linear. In 1941, Kolmogorov attempted to model turbulence in the atmosphere using a statistical approach. The Kolomogorov theory of turbulence is based on the assumption that wind velocity fluctuations are approximately locally homogeneous and isotropic random fields for scales less than the largest wind eddies. (Beland, 1993; Beckers 1993).

How do phase variations due to atmospheric turbulence affect the intensity of the incident electro-magnetic wave? Assuming the incoming electric field portion of the electro-magnetic wave E is proportional to with the angular frequency and t time, the wave equation

reduces to

where k is the wavenumber for propagation in free space, n is the index of refraction and the dispersion relation holds. (Note that the wavenumber for propagation through the atmosphere is .)

This equation cannot be solved exactly, so we approximate the solution using a perturbation expansion of n and E. This assumes that for the area of the sky we are interested in, the index of refraction undergoes slow, small perturbations due to the atmospheric turbulence. Let where is the incident electric field and is the scattered field. where .

Dropping the second order term,

Putting in the perturbation to E

Dropping the small term and using

equation 22 becomes

This can be solved in terms of using Green's function for the wave equation, giving

integrating over the scattering volume between source and telescope. (Beland, 1993).

However, this solution is only valid for very weak perturbations of E and the integral over the scattering volume between the source and telescope is not very convenient since the effects of phase variations are not obvious. A less limiting method is the Rytov method of smooth perturbations. Here E is written as

where and , A is the amplitude and S is the phase of E. Lutomirski and Yura, using an extended Huygens-Fresnel theory find

here integrating over a surface.

The intensity of the incoming wavefront will tell us how the phase fluctuations degrade the resolution.

The mutual coherence function (MCF) in the focal plane of the telescope is given by and is equal to where is the transverse coherence length. A spatially coherent wavefront will have its spatial coherence degraded to after passing through turbulence.

Most astronomical applications translate this spatial mutual coherence function to the modulation transfer function (MTF) in the spatial frequency domain. The modulation transfer function where f is the focal length, is the spatial frequency (cycles/length), is the wavelength of light, and is the atmospheric coherence length or Fried parameter. is about 10 cm for a vertical path for visible wavelength and characterizes the effect of turbulence on the incoming wavefront. Since optical turbulence blurs out point source functions, there is a cutoff spatial frequency and gives the limit of resolution due to optical turbulence. (Beland, 1993; Beckers, 1993.)

The diffraction limit of resolution for 4m telescope at 500 nm is given by equation 17

Assuming , the angular resolution due to atmospheric turbulence R is

So turbulence in this case degrades the resolution by a factor of 100!

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