Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

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 ). ...

Next: Stars without Periods Up: Other Stars Previous: Stars with Highly . ... However, due to lower signal to noise their periods are less secure. ... This could be interpreted as a continuous distribution with statistically insignificant deviations which give the appearance of gaps or a real gap. ... When the distributions of periods greater five days are compared for the ONC stars and those near Orionis the KS test gives a 47% probability of these distributions being drawn from the same population. ...

A Test of Galaxy Evolutionary Models Via Angular Sizes M. Im S. Casertano, R. E. Griffiths, & K. U. Ratnatunga (The Johns Hopkins University) The relationship between angular size, magnitude, and redshift of faint galaxies is explored as a potential tool to distinguish between different galaxy evolutionary models. ... The mild lumi­ nosity evolution model predicts more luminous galaxies of large angular size at high redshift, as does a standard no evolution model. ... 25) with redshift higher than z ? ...

... 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 . ...

... 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. ...

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. ...

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. ...

... You are here: start €Ё correlator €Ё distribution . ... Distribution of output data to PIs . ... You can make your own directory for distributing data to PIs (or geodetic analysts) on cuppa21 under: /data/corr/corrdat/DistributeData/ . ... To copy FITS files etc. from the correlator output area to a folder on CloudStor+ (can also just use scp or rsync if preferred): gloPut7T.sh -m VX021A.FITS /data/corr/corrdat/vx021a hbignall@cuppa21 /data/corr/corrdat/DistributeData/hayley/ownCloud/VLBI/vx021a . ...

... 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...

... 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. ...

... According to the most popular cosmological paradigm, the greater part of the galaxy mass is accumulated in the dark matter halo. ... The polar ring galaxies (PRGs) reveal external rings or disks of gas, dust and stars rotating in a plane roughly perpendicular to the disk of the central galaxy. ... The shape of the dark halo in the model was chosen so as to achieve the best fit to the observed rotation of both galaxies themselves and their polar rings. ... The SPRC-7 galaxy. ...

The project of the informational system creation on the problem of evolution of radio galaxies, as a part of the "Big Trio" project aimed on studing of distant radio galaxies, is designed. This system allows a user to operate with simulated curves of spectral energy distributions (SED) to estimate ages and redshifts by photometry data. Authors use SEDs of several models for different types of galaxies. ... The HTTP and e-mail access is organized to this system. ...

... One of the most widely used tools of Fourier analysis is the Parseval theorem. It enables the experimentalist to view how the `energy' in the signal is distributed among frequencies. The Fast Fourier Transform (FFT) algorithms have made power spectra one of the obvious diagnostics tools during data acquisition, and energy maps are a versatile alternative. ... The result is an energy map (Fig. 9), showing the distribution of energy corresponding to the wavelet map (Fig. ...

... Up: Software Systems and Tools . ... The Starlink Software is a collection of astronomical packages and utilities comprising over 120 separate components. When built, the system needs between 500 and 650 MB disk space (without source) making it ideal for distribution on CD-ROM. Each component has been individually packaged into an easy-to-install bundle for users to obtain over the Internet via a ``point and click'' WWW interface from the Starlink Software Store. ...

... To see how this is done, it helps to visualise the colours as points inside a cube with edges 1 unit in length. ... The task of allocating these colours is equivalent to constructing 256 boxes inside the cube, each box to contain a subset of the thousands of colour points. ... At present the boxes are allocated so that they all tend to be of equal size, but it may make more sense to allocate them so that they all tend to contain equal numbers of points. ...

... 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...

These lesson introduces you to the use of uncertainties. ... It introduces probability distribution functions, the Gaussian Distribution, hypothesis testing and model fitting. This lesson introduces you to the different types of uncertainty, and how you can estimate them from the scatter in your measurements, or from knowledge of your experimental set-up. ... It also covers averaging and how that affects uncertainties. Back Main Lab-Skills Page . ...

Where and how are we looking for evidence of life? ... Because the universe is an immense place, it makes sense to search for evidence of life in more than one way. In addition to focusing on what we know about life on Earth, especially in extreme environments, astrobiology currently comprises three basic types of searches in space, each employing different technologies, looking in different places, and expecting to find different kinds of data: . ... The search types ? ... Extrasolar Planets vs. ...

... St Petersburg 23, September 2014 1 Motivation · Origin of Martian moons? ... Considered error sources: ­ Phobos a priori ephemerides; ­ Phobos a priori GM value; ­ measurements noise; ­ different strategies; · Methods: ­ real data analysis; ­ simulations. ... St Petersburg 23, September 2014 8 Simulations: sensitivity of the measurements to the a priori GM value Simulations: zero noise+ IMCCE a priori ephemerides +GMPH = 7.16 * 105 m3/sec2. ... St Petersburg 23, September 2014 14 Thank you! ...