Abstract

The maximum of the probability density distribution of phase fluctuations in the earth’s atmosphere, as a function of point separation, was measured visually in white light for starlight observed from the ground with a 1.5 m astronomical telescope. A wave-front folding interferometer was used.

© 1976 Optical Society of America

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Corrections

J. B. Breckinridge, "Errata: Measurement of the amplitude of phase excursions in the earth’s atmosphere," J. Opt. Soc. Am. 66, 981_2-981 (1976)
https://www.osapublishing.org/josa/abstract.cfm?uri=josa-66-9-981_2

References

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  1. F. Dyson, J. Opt. Soc. Am. 65, 551 (1975).
    [Crossref]
  2. Proceedings of the Optical Society of America Topical Meeting on Imaging in Astronomy, Boston, Mass., June 1975.
  3. J. B. Breckinridge, J. Opt. Soc. Am. 65, 755 (1975).
    [Crossref]
  4. A. Labeyrie, Nouv. Rev. Opt. 5, 141 (1974).
    [Crossref]
  5. R. H. Dicke, Astrophys. J. 198, 605 (1975).
    [Crossref]
  6. J. C. Dainty and R. Scaddan, Mon. Not. R. Astron. Soc. 170, 519 (1975).
  7. C. Roddier and F. Roddier, J. Opt. Soc. Am. 63, 661 (1973).
    [Crossref]
  8. M. Bertolotti, M. Carnevale, L. Muzii, and D. Sette, J. Opt. Soc. Am. 60, 1603 (1970).
    [Crossref]
  9. R. G. Buser, J. Opt. Soc. Am. 61, 488 (1971).
    [Crossref]
  10. D. L. Fried, J. Opt. Soc. Am. 55, 1427 (1965).
    [Crossref]
  11. D. L. Fried and G. E. Mevers, Appl. Opt. 13, 2620 (1974).
    [Crossref] [PubMed]
  12. C. E. Coulman, Sol. Phys. 34, 491 (1974).
    [Crossref]
  13. C. Roddier and F. Roddier, J. Opt. Soc. Am. 65, 664 (1975).
    [Crossref]

1975 (5)

1974 (3)

C. E. Coulman, Sol. Phys. 34, 491 (1974).
[Crossref]

D. L. Fried and G. E. Mevers, Appl. Opt. 13, 2620 (1974).
[Crossref] [PubMed]

A. Labeyrie, Nouv. Rev. Opt. 5, 141 (1974).
[Crossref]

1973 (1)

1971 (1)

1970 (1)

1965 (1)

Bertolotti, M.

Breckinridge, J. B.

Buser, R. G.

Carnevale, M.

Coulman, C. E.

C. E. Coulman, Sol. Phys. 34, 491 (1974).
[Crossref]

Dainty, J. C.

J. C. Dainty and R. Scaddan, Mon. Not. R. Astron. Soc. 170, 519 (1975).

Dicke, R. H.

R. H. Dicke, Astrophys. J. 198, 605 (1975).
[Crossref]

Dyson, F.

Fried, D. L.

Labeyrie, A.

A. Labeyrie, Nouv. Rev. Opt. 5, 141 (1974).
[Crossref]

Mevers, G. E.

Muzii, L.

Roddier, C.

Roddier, F.

Scaddan, R.

J. C. Dainty and R. Scaddan, Mon. Not. R. Astron. Soc. 170, 519 (1975).

Sette, D.

Appl. Opt. (1)

Astrophys. J. (1)

R. H. Dicke, Astrophys. J. 198, 605 (1975).
[Crossref]

J. Opt. Soc. Am. (7)

Mon. Not. R. Astron. Soc. (1)

J. C. Dainty and R. Scaddan, Mon. Not. R. Astron. Soc. 170, 519 (1975).

Nouv. Rev. Opt. (1)

A. Labeyrie, Nouv. Rev. Opt. 5, 141 (1974).
[Crossref]

Sol. Phys. (1)

C. E. Coulman, Sol. Phys. 34, 491 (1974).
[Crossref]

Other (1)

Proceedings of the Optical Society of America Topical Meeting on Imaging in Astronomy, Boston, Mass., June 1975.

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Figures (1)

FIG. 1
FIG. 1

Plot of the visually measured fringe amplitude in waves as a function of pupil point separation in meters across the 1.5 m McMath Solar Telescope at Kitt Peak. Source was a star near the zenith. Points on the graph are averages of 3 stars all observed on 4 different nights near the zenith. Straight line shows a 5 6 power dependence. Seeing was approximately 3 arc-sec.

Tables (1)

Tables Icon

TABLE I Measured peak-to-peak fringe amplitude and peak-to-peak total physical motion (1) required for active optics compensation as a function of point separation (d) at the telescope pupil. Average of 3 nights observations on each of 4 stars.

Equations (3)

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l = λ ( f / 2 ) 2 .
D ( r ) = [ ϕ ( X ) - ϕ ( X 1 ) ] 2 = 6.88 ( r / r 0 ) 5 / 3 ,
( 2 π ) ( 1 2 f ) / N = [ 6.88 ( d / r 0 ) 5 / 3 ] 1 / 2