... Calculations of at least two runs with different values of a parameter are required in order to discover to what extent the results depend on the , if at all. ... In order to study how the final statistical distributions depend on the initial functions, the method of Green functions is used. ... Then we can restore any distribution on this parameter (with a certain accuracy) by summing the results for each interval with the appropriate weight. ...

Distribution of the analyzed SEPs with different >100 MeV proton fluxes ( J 100 ) at the microwave flux density plane ' S 9 vs. ... 1) General correspondence takes place between intensities of microwave bursts and proton fluxes - J 100 increases when S 9 and S 15 rise. ... 3) Powerful microwave bursts ( S 9 , S 15 >3000-10000 sfu ) with hard radio spectra ( S 9 < S 15 ) correspond to majority of powerful proton fluxes ( J 100 >10 pfu ). ...

... Posts tagged ?Pareto distribution? ... Posted by hlee . ... Tags: Classification , covariance , FARIMA , Fisher information , GL , GRB , Levy , light curve , limb darkening , ML , Pareto distribution , quasars , solar flare , standard candle , tessellation , time series , VO , void . ... 1 Comment . ... ArXiv] Pareto Distribution? ... 4 Comments . ... From arxiv/astro-ph, arXiv:0706.2590v1 Extreme Value Theory and the Solar Cycle by Ramos, A. This paper might drag a large attention from CHASC...

Yu.V.Lunyova, A.F.Kholtygin . Chemical evolution of the system of galactic planetrary nebulae , Astrophysics , 45 , 451-463 (2002) . Chemical evolution of the system of galactic planetary nebulae beginning from the early age of the Galaxy is investigated. We calculate radial and vertical abundance gradients of C, N, O, Ne, Ar, Cl and S depending of different ages of the central star of the nebula. It have been founded statistically significant dependence of abundance gradients with the age of central star.

This is a tabulation of interstellar dust scattering properties dertermined from observations of various astrophysical objects (eg., ... Almost all studies in this field aim to determine the single scattering albedo (a) and scattering phase function asymmetry (g = <cos( )>) as different wavelengths. ... Plot Details . ... Plot details links to a page describing the studies included in the plot, the radiative transfer model used in each study, and an ascii listing of data plotted. ...

Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

... Using the central limit theorem, the total noise can be approximated by a Gaussian or normal distribution which has the frequency function : . ... where is the mean intensity of the source. ... In the statistical analysis of the probability distribution of data several estimators based on moments are used. ... For a normal distribution, these moments are and while for a Poisson distribution are and . Besides these moments other estimators are used to describe a distribution e.g. median and mode . ...

Scale-heights of the Galactic disk subsytems with different ages and metallicities . V.Marsakov & Yu. ... It is based on the fact, that all stars cross the disk plane several times during their Galactic orbital period. ... We have used our representative sample of nearby disk F2-G2 stars Marsakov & Shevelev (1995) in which fundamental stellar parameters was determined on the basis of published date on uvby-photometry, proper motion and radial velocities. ... Marsakov V.A., Shevelev Yu.G. Bull. ...

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

... The distribution of galactic RCB stars is controversial. Several authors have argued that they belong to a thick galactic disk, and are thus old Population I stars. However, they may alternatively belong to the even older galactic bulge (Population II). ... In either case, the populations are sufficiently old that RCB stars must have relatively low masses ( ). ... These are the only RCB stars for which a distance is known and hence for which an absolute magnitude can be deduced. ...

... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Australian Square Kilometre Array Pathfinder . Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

... Bisnovatyi-Kogan, Gennady S.; Merafina , Marco; Vaccarelli , Maria Rosaria; Spherically Symmetric Stellar Clusters with Anisotropy and Cutoff Energy in Momentum Distribution. ... We construct numerical models of spherically symmetric Newtonian stellar clusters with anisotropic distribution functions. ... Models of spherically symmetric relativistic stellar clusters with anisotropic distribution functions in relativistic regime are described by using Maxwellian distribution function with energy...

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

To construct two-dimension distribution of minor planets user should specify elements/ parameters/ function that will be plotted as abscissas and ordinates. In three-dimension case one should add to them the element plotted on Z axis. ... Though you may choose elements plotted along different axes at will, often there is good reason to plot such elements as a, n, or n" along X axis (two-dimension distributions) and to plot them along Y axis in three-dimension case. ...

If the calculated chi-squared statistic exceeds a tabled value for the appropriate number of degrees of freedom, then observed values are significantly different from expected values at the confidence level indicated by p. For one degree of freedom: . p=0.05, 3.84; p=0.025, 5.02; p=0.01, 6.64; p=0.005, 7.88 . For two degrees of freedom: . ... For three degrees of freedom: . ... For four degrees of freedom: . ... For five degrees of freedom: . ...

Download Izmccd (~2.7 MB). ... a) a choice of the best mode of measurements of stars and objects ("Properties/Measurement"), . b) a choice of reference stars. ... 1) necessity of presence on an image of a plenty of stars (we recommend to apply this mode, if on the frame of reference stars is more 100) . ... Sx and Sy depend from residuals at all reference stars (reference stars are marked by blue color). ... These residuals are the image of the star a minus function of a profile for each pixel. ...

... Dept. for Physics of Stars&Galaxies . ... Astronomical Calendar . ... History of MAO . ... БЂ“ 2013. ... Zakhozhay O. and Vorobyov E.I. The signatures of disk fragmentation in spectral energy distributions // Proceedings of the conference Hot Planets and Cool Stars, Garching, November 12-16, 2012. ... Zakhozhay O.V., Vorobyov E.I. Spectral energy distributions of fragmenting protostellar disks // Formation, detection, and characterization of extrasolar habitable planets Proceedings IAU Symposium No....

... The task calculates an average RMF over the spatial region used to extract the source spectrum. ... Essentially a grid is placed over the source region and the redistribution parameters calculated at each point. ... By means of command line parameters the averaging may be performed assuming that the flux distribution is that of the point spread function (PSF), a flat uniform distribution or it may be defined explicitly by supplying the task with an image containing the source region. ...

... The distribution of redshifts among the DXRBS FSRQs identified so far (Figure 3) is quite similar to that of the 1 Jy and S4 samples. ... A more thorough comparison will have to await completion of our survey and the convolution of the redshift distribution with the WGACAT sky coverage. As has already been mentioned by Hook et al. (1996), selecting flat-spectrum sources is an efficient way of finding high-redshift, radio-loud quasars. ...