scholarly journals STATISTICAL ANALYSIS OF ATOM-PROBE DATA (II) : THEORETICAL FREQUENCY DISTRIBUTIONS FOR PERIODIC FLUCTUATIONS AND SOME APPLICATIONS

1988 ◽  
Vol 49 (C6) ◽  
pp. C6-439-C6-444 ◽  
Author(s):  
P. AUGER ◽  
A. MENAND ◽  
D. BLAVETTE
Keyword(s):  
Statistical Analysis ◽  
Atom Probe ◽  
Frequency Distributions ◽  
Theoretical Frequency ◽  
Periodic Fluctuations

STATISTICAL ANALYSIS OF ATOM PROBE DATA

1986 ◽  
Vol 47 (C7) ◽  
pp. C7-489-C7-494
Author(s):  
L. V. ALVENSLEBEN ◽  
R. GRÜNE ◽  
A. HÜTTEN ◽  
M. OEHRING
Keyword(s):  
Statistical Analysis ◽  
Atom Probe

ON THE STATISTICAL ANALYSIS OF ATOM PROBE DATA

1987 ◽  
Vol 48 (C6) ◽  
pp. C6-559-C6-564 ◽  
Author(s):  
M. G. Hetherington ◽  
M. K. Miller
Keyword(s):  
Statistical Analysis ◽  
Atom Probe

scholarly journals IX. Mathematical contributions to the theory of evolution.—XIX. Second supplement to a memoir on skew variation

1916 ◽  
Vol 216 (538-548) ◽  
pp. 429-457 ◽  
Keyword(s):  
Standard Deviation ◽  
Homogeneous Material ◽  
Fourth Moment ◽  
Frequency Distributions ◽  
Theory Of Evolution ◽  
Theoretical Frequency ◽  
Moment Coefficient ◽  
The Mean ◽  
The Moment ◽  
True Values

In a memoir presented to the Royal Society in 1894, I dealt with skew variation in homogeneous material. The object of that memoir was to obtain a series of curves such that one or other of them would agree with any observational or theoretical frequency curve of positive ordinates to the following extent :—(i) The areas should be equal; (ii) the mean abscissa or centroid vertical should be the same for the two curves; (iii) the standard deviation (or, what amounts to the same thing, the second moment coefficient) about this centroid vertical should be the same, and (iv) to (v) the third and fourth moment coefficients should also be the same. If μ s be the s th moment coefficient about the mean vertical, N the area, x ¯ be the mean abscissa, σ = √ μ 2 the standard deviation, β 1 = μ 3 2 / μ 2 3 , β 4 = μ 4 / μ 2 2 , then the equality for the two curves of N, x ¯ , σ, β 1 and β 2 leads almost invariably in the case of frequency to excellency of fit. Indeed, badness of fit generally arises from either heterogeniety, or the difficulty in certain cases of accurately determining from the data provided the true values of the moment coefficients, e. g ., especially in J- and U-shaped frequency distributions, or distributions without high contact at the terminals ; here the usual method of correcting the raw moments for sub-ranges of record fails. Having found a curve which corresponded to the skew binomial in the same manner as the normal curve of errors to the symmetrical binomial with finite index, it occurred to me that a development of the process applied to the hypergeometrical series would achieve the result I was in search of, i. e ., a curve whose constants would be determined by the observational values of N, x ¯ , σ, β 1 and β 2 .

scholarly journals Species frequency distribution as a function of the surface area

2014 ◽  
Vol 53 (1) ◽  
pp. 87-98
Author(s):  
Anna J. Kwiatkowska
Keyword(s):  
Statistical Analysis ◽  
Surface Area ◽  
Frequency Distribution ◽  
Point Of View ◽  
Sample Plot ◽  
Statistical Point ◽  
Frequency Distributions ◽  
Species Frequency

Paper deals with the results of statistical analysis of the type of frequency distribution of species occuring in the field layers of two forest phytocoenoses. In the both cases frequency distributions were ranged out for the surface area of 1, 2, 4, 8, 16, 32 and 64 m<sup>2</sup>. The types of frequency distributions were determined on the grounds of the values of Fisher's and Pearson's K coefficients. Analysed distributions were classified into Pearson's system. Also the size of the sample plot at which the empirical frequency distributions were symetrical, from the statistical point of view, nad where they were U-shaped was determined.

Lidar-Derived Distribution of Cloud Vertical Location and Extent

1995 ◽  
Vol 34 (1) ◽  
pp. 107-120 ◽  
Author(s):  
A. I. Carswell ◽  
A. Fong ◽  
S. R. Pal ◽  
I. Pribluda
Keyword(s):  
Statistical Analysis ◽  
Frequency Distributions ◽  
Geometrical Properties ◽  
Cloud Properties ◽  
Vertical Location ◽  
Other Information ◽  
Relationship Of ◽  
The Relationship ◽  
Cloud Thickness ◽  
532 Nm

Abstract This paper summarizes the results of a statistical analysis of lidar-determined cloud geometrical properties measured during the 1989 and 1991 campaigns of the Experimental Cloud Lidar Pilot Study. Useful lidar descriptors are introduced to specify the bottom-, top-, and midcloud altitudes. These are used to describe the behavior of cloud vertical location and vertical extent during several months of observations using a dual wavelength (1064 and 532 nm) Nd:YAG lidar at Toronto. Frequency distributions of cloud height and cloud thickness are presented and the relationship of the lidar descriptors to cloud properties are discussed. These data are compared with other information on cloud geometry available in the literature.

scholarly journals Applying Multivariate Statistical Analysis to Atom Probe Tomography

2010 ◽  
Vol 16 (S2) ◽  
pp. 1858-1859 ◽  
Author(s):  
C Parish ◽  
C Capdevila ◽  
MK Miller
Keyword(s):  
Statistical Analysis ◽  
Multivariate Statistical Analysis ◽  
Atom Probe Tomography ◽  
Atom Probe ◽  
Multivariate Statistical

Extended abstract of a paper presented at Microscopy and Microanalysis 2010 in Portland, Oregon, USA, August 1 – August 5, 2010.

scholarly journals Spin rates of V-type asteroids

2020 ◽  
Vol 643 ◽  
pp. A117
Author(s):  
Dagmara Oszkiewicz ◽  
Volodymyr Troianskyi ◽  
Dóra Föhring ◽  
Adrián Galád ◽  
Tomasz Kwiatkowski ◽  
...  
Keyword(s):  
Statistical Analysis ◽  
Solar System ◽  
Critical Density ◽  
Rotational Frequency ◽  
Significant Excess ◽  
Frequency Distributions ◽  
The Family ◽  
Detailed Statistical Analysis ◽  
Yorp Effect ◽  
Insight Into

Context. Basaltic V-type asteroids play a crucial role in studies of Solar System evolution and planetesimal formation. Comprehensive studies of their physical, dynamical, and statistical properties provide insight into these processes. Thanks to wide surveys, currently there are numerous known V-type and putative V-type asteroids, allowing a detailed statistical analysis. Aims. Our main goal is to analyze I corrected for US language conventions in this paper the currently available large sample of V-type spin rates, to find signatures of the non-gravitational Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect among the different V-type populations, and to estimate the spin barrier and critical density for V-type asteroids. Our intention is to increase the pool of information about the intriguing V-types. Methods. We collected rotational periods from the literature for spectrally confirmed V-types, putative V-types, and Vesta family members. Through spectroscopic observations we confirmed their taxonomic type and verified the high confirmation rates of the putative V-types. We combined the collected periods with periods estimated in this manuscript and produced rotational frequency distributions. We determined the spin barrier in the frequency–light curve amplitude space for V-type asteroids. Results. We analyzed rotational periods of 536 asteroids in our sample. As expected, due to the small size of the objects analyzed, the frequency distributions for the Vesta family and the V-types outside the family are inconsistent with a Maxwellian shape. The Vesta family shows an excess of slow-rotators. V-types outside the family show an excess of both slow and fast rotators. Interestingly, we found that the population of V-types outside the Vesta family shows a significant excess of fast rotators compared to the Vesta family. The estimated critical density for V-type asteroids exceeds ρc = 2.0 g cm−3, which surpasses the previous estimates. Conclusions. We demonstrated that V-type asteroids have been influenced by the thermal radiation YORP effect and that their critical spin rate is higher than for C-type asteroids. The population of V-types outside the Vesta family shows a significant excess of fast rotators compared to the Vesta family. We hypothesize that the objects that evolved from the Vesta family though the Yarkovsky drift are also more susceptible to the YORP effect. Objects for which YORP has not yet had enough time to act and those that are more YORP resistant will be left in the family, which explains the relatively small proportion of fast rotators being left. The YORP timescale must thus be similar to the migration timescale for those objects.

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