Statistical Properties of Estimates of the Moments of Laser Scintillation

Frehlich, Rod; Churnside, James H.

doi:10.1080/09500348914551761

Cited by 8 publications

(3 citation statements)

References 24 publications

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“…A more fundamental observational problem is that an enormous number (millions) of independent samples are needed in order to obtain statistically significant determinations of higher moments (Ben-Yosef and Goldner 1988;Frehlich and Chumside 1989;Goldner and Ben-Yosef 1988;Hill and Chumside 1988). These authors argue that, for reasonable and practical sample sizes, the correct estimation of such values is improbable or even impossible.…”

Section: Can Scintillation Statistics Be Determined At All?mentioning

confidence: 99%

“…Since higher moments m k are strongly dependent on such rare events, the finite integration time usually causes such moments to be underestimated. From numerical simulations, Frehlich and Chumside (1989) show how the effects of amplifier saturation become signifi-cant when the saturation irradiance is less than the median of the maximum irradiance value for a given sample size N, and a model PDF.…”

Section: Can Scintillation Statistics Be Determined At All?mentioning

confidence: 99%

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Atmospheric Intensity Scintillation of Stars, I. Statistical Distributions and Temporal Properties

Dravins¹,

Lindegren²,

Mezey³

et al. 1997

PASP

102

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Stellar intensity scintillation in the optical was extensively studied at the astronomical observatory on La Palma (Canary Islands). Photon-counting detectors and digital signal processors recorded temporal auto-and cross-correlation functions, power spectra, and probability distributions. This first paper of a series treats the temporal properties of scintillation, ranging from microseconds to seasons of year. Previous studies, and the mechanisms producing scintillation are reviewed. Atmospheric turbulence causes 'flying shadows' on the ground, and intensity fluctuations occur both because this pattern is carried by winds, and is intrinsically changing. On very short time scales, a break in the correlation functions around 300 ¡¿s may be a signature of an inner scale (=3 mm in the shadow pattern at wind speeds of 10 m s -1 ). On millisecond time scales, the autocorrelation halfwidth decreases for smaller telescope apertures until -5 cm, when the 'flying shadows' become resolved. During any night, time scales and amplitudes evolve on scales of tens of minutes. In good summer conditions, the flying-shadow patterns are sufficiently regular and long-lived to show anti-correlation dips in autocorrelation functions, which in winter are smeared out by apparent wind shear. Recordings of intensity variance together with stellar speckle images suggest some correlation between good (angular) seeing and large scintillation. Near zenith, the temporal statistics (with up to twelfth-order moments measured) is best fitted by a Beta distribution of the second kind (F-distribution), although it is well approximated by log-normal functions, evolving with time.

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Section: Can Scintillation Statistics Be Determined At All?mentioning

confidence: 99%

Section: Can Scintillation Statistics Be Determined At All?mentioning

confidence: 99%

Atmospheric Intensity Scintillation of Stars, I. Statistical Distributions and Temporal Properties

Dravins¹,

Lindegren²,

Mezey³

et al. 1997

PASP

102

View full text Add to dashboard Cite

show abstract

“…This method, summarized in Section 3, can be applied to any scintillation regime from a very low to a very strong one, because low-order moments can be accurately estimated from experimental data. Recall that, apart from the case of low scintillation, the number of uncorrelated data that can be collected under stationary conditions is generally not enough to correctly estimate intensity moments of order greater than two [5,6]. On the other hand, fractional moments of order less than two can be correctly estimated.…”

Section: Introductionmentioning

confidence: 99%