Abstract

The mutual coherence function (MCF) of the complex amplitude of stellar light waves perturbed by atmospheric turbulence has been determined interferometrically. Results are in good agreement with horizontal laser-beam determinations. Stellar measurements provide quantitative estimations of seeing conditions for astronomical observations.

© 1973 Optical Society of America

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References

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  1. M. Bertolotti, L. Muzii, and D. Sette, J. Opt. Soc. Am. 60, 1603 (1970).
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  5. J. Bufton and S. H. Genatt, Astron. J. 76, 378 (1971).
    [Crossref]
  6. A. T. Young. Astron. J. 72, 747 (1967).
    [Crossref]
  7. E. Moroder and A. Righini, Astron. Astrophys. 23, 307 (1973).
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  9. R. E. Hufnagel and N. R. Stanley, J. Opt. Soc. Am. 54, 52 (1964).
    [Crossref]
  10. V. I. Tatarski, Wave Propagation in a Turbulent Medium (Dover, New York, 1961).

1973 (1)

E. Moroder and A. Righini, Astron. Astrophys. 23, 307 (1973).

1971 (3)

1970 (2)

1967 (1)

A. T. Young. Astron. J. 72, 747 (1967).
[Crossref]

1966 (1)

1964 (1)

Ackley, M. H.

Bertolotti, M.

Bolstad, J. O.

Bouricius, G. M. B.

Bufton, J.

J. Bufton and S. H. Genatt, Astron. J. 76, 378 (1971).
[Crossref]

Buser, R. G.

Clifford, S. F.

Fried, D. L.

Genatt, S. H.

J. Bufton and S. H. Genatt, Astron. J. 76, 378 (1971).
[Crossref]

Hufnagel, R. E.

Moroder, E.

E. Moroder and A. Righini, Astron. Astrophys. 23, 307 (1973).

Muzii, L.

Ochs, G. R.

Righini, A.

E. Moroder and A. Righini, Astron. Astrophys. 23, 307 (1973).

Sette, D.

Stanley, N. R.

Tatarski, V. I.

V. I. Tatarski, Wave Propagation in a Turbulent Medium (Dover, New York, 1961).

Wessely, H. W.

Young, A. T.

A. T. Young. Astron. J. 72, 747 (1967).
[Crossref]

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Figures (4)

Fig. 1
Fig. 1

Michelson interferometer at the telescope focus. O, telescope objective; M1, M2 interferometer mirrors; S1, S2, S3, beam splitters; A, artificial star for autocollimation; L1, L2, convergent lenses; D1, D2, diaphragms in the objective image plane; D1, D2, diaphragms in the sky image plane; PMI, PM2, photomultipliers; O, O, images of the objective.

Fig. 2
Fig. 2

Scanning of the star across the fringes for d = 2.5 cm. The amplitude variation is due to the finite spectral bandwidth Δλ. The interval between two contiguous maxima corresponds to a 140 μm (4) displacement of the star on the focal plane.

Fig. 3
Fig. 3

Observed MCF M (d) for two different stars. A, Aldebaran (z = 30°); B, Altaïr (z = 70°).

Fig. 4
Fig. 4

A, B, Logarithm of the M (d) functions shown on Fig. 3, plotted on a log log scale. A, B, same curves after a zenith-angle correction cosz ; 5/3 s, theoretical straight line with a 5/3 slope.

Equations (8)

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i ( r , t ) = | V ( r , t ) + V ( r + d , t ) e 4 i π a θ / λ | 2 ,
I 1 = s i ( r , t ) d r = s | V ( r , t ) | 2 d r + s | V ( r + d , t ) | 2 d r + 2 cos ( 4 π a θ / λ ) Re s V ( r , t ) V * ( r + d , t ) d r .
I 1 I 2 = 4 cos ( 4 π a θ / λ ) Re s V ( r , t ) V * ( r + d , t ) d r
I 1 + I 2 = 4 s | V ( r , t ) | 2 d r .
I 1 I 2 I 1 + I 2 = cos 4 π a θ / λ ( Re s V ( r , t ) V * ( r + d , t ) d r / s | V ( r , t ) | 2 d r )
M ( d ) = V ( r , t ) V * ( r + d , t ) | V ( r , t ) | 2
M ( d ) = exp 1 2 D ( d ) ,
D ( d ) = 2.91 k 2 sec z d 5 / 3 0 C N 2 d h ,