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. ...

... CentralProcessor 0.11 documentation . Calibration and Imaging Documentation . The cmodel pipeline task is responsible for extracting a local sky model (LSM) from the global sky model (GSM) and building an image from the components and/or images resulting from the request. ... MPI wrapper> cmodel -c config.in . ... None . ... If Cmodel.gsm.database is set to asciitable then a row/column (space separated) file is used as the global sky model source. ... cmodel (Model Image Generator) . ...

... Bojan Nikolic web pages (r. 329) . ... We present a Bayesian approach to calculating the coefficients that convert the outputs of ALMA 183 GHz water-vapour radiometers into estimates of path fluctuations that can be used to correct the observed interferometric visibilities. ... Inference of Coefficients for Use in Phase Correction . ... Simulating Atmospheric Phase Errors, Phase Correction and the Impact on ALMA Science . ... Copyright 2005 -- 2016, Bojan Nikolic feedback welcome ...

... The Radon transform (also known as the Hough transform) is formulated as a family of line integrals through a two-dimensional function. ... The Radon transform provides us with a simple means of computing the FF plane of the autochirplet transform, by using the Wigner distribution, and arriving at a transform space that tells us basically the same information as the chirplet FF-plane, except that we benefit from the greater resolution of the Wigner distribution. ...

... The PSF is stored as a radial distribution in the CCF component PSF1DRB. ... The radial width of the PSF is stretched by the factor f by multiplying the radial bin limits with f : . The stretching factor f is calculated for the specified field position (rawX, rawY) from a 3rd order polynomial. (35) . ... calculate the minimum distance r of the pixel to the PSF centre (rawX, rawY) . calculate the maximum distance r of the pixel to the PSF centre (rawX, rawY) . ... normalize PSF map to 1 . ...

... Minute Values of Geomagnetic Field Components . ... AA 1868 - Present (3 hourly and daily) (monthly) (yearly) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) KP_AP 1932 - Present (3 hourly and daily) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) AE_HV 1957-75, 78-88 (hourly) AE_MIN 1978-881-6;198903;1990-94 (minute) DST 1957 - Present (hourly) PC 1975 - Present (15-minute) AMANAS 1959 - Present (3 hourly and daily) KMKNKS 1983 - Present (3 hourly) . ...

In this chapter we will consider an example of visual expert system written on the Actor Prolog language. ... There are a lot of methods of oil field bed stimulation that increase output of the oil production: thermal, physical-chemical, gas, microbiological, and others. ... Fig. ... The Top-Most diagram consists of three blocks: the "Describe parameters of hydrocarbon field" block, the "Check adaptability of existed methods of oil production" block, and the "Display solution" block. ... Gas methods. ...

The magnetic mapping is fulfilled by the magnetic field line tracing from the satellite position up to the Ionosphere (stop trace at the altitude 110 km). ... As a rule the Tsyganenko [1987] external magnetic field model and IOPT = 3 (Kp = 2) are used. ... The output file includes the following information: . ... For example the file with name aa9610d1.geo contains the information corresponding to the aposteriory magnetic mapping for INTERBALL Auroral Probe for the first decade of October 1996. ...

Next: Simulated Results with Up: Assessment of Methods Used Previous: Introduction . ... Then one has to use regularized inversion methods in order to obtain approximate and sensible solutions. ... All these methods contain a free parameter which is the so-called regularization parameter; in the case of method ( ) this is a smoothing of the higher spatial frequencies; for the methods ( ) - ( ), it is the number of iterations. ... In the case of method ( ) the iteration scheme is given by . ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

Following designations of elements/ parameters are used in AMPLE. ... mean anomaly . ... Node . ... Apart conventional orbital elements AMPLE gives possibility to calculate for each minor planet the following often used functions: . ... MOID . ... To calculate MOID user should order the name or the number of the major or minor planet through dialog. ... To calculate CT user should order the name or the number of the major or minor planet through dialog as it is proposed for MOID calculation. ...

... 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...

... Archives . ... ArXiv] Google Sky, Sept. 05, 2007 . ... Inference for mixtures of symmetric distributions by Hunter, Wang, and Hettmansperger, Annals of Statistics, 2007, Vol.35(1), pp.224-251. ... Although math.st:0708.0499 did not discuss spectral line fitting, it offers a nice review on identifiability when inferencing for mixtures of symmetric distributions. ... Fitting mixture of normal distributions suffers from identifiability issues. 09-09-2007, 11:51 pm . ... Chandra Blog . ...

CIMA is more than just the observing tool - in fact, the observing tool is just a part of a bigger package called the CIMA software package. ... There is also a another package called the CIMA WAPP software which contains the WAPP software, the special Tcl/Tk interpreter used by CIMA and support libraries. ... All CIMA software components recognize the following general options that are part of the CIMA version selection system: . ... The select_cima script can be used to set up a default version. ...

... Polar Cap Potential . ... The solar wind propagation delay time calculation used here is conceptually similar to the T(IMF) calculation in Kelly, et al. ... The older continuous data are from key parameter data files. ... Note: Very high values of Solar Wind Speed, Solar Wind Pressure, IMF Magnitude and Bz, and Polar Cap Potential are likely indications that WIND has reentered the Earth's magnetosphere; such data is not indicative of solar wind conditions or impending severe geomagnetic disruption. ...

The reduction of a given magnitude m to bt is given by: . bt = a.m + b + c.(logr25 - <logr25>) . ... e.(logd25 - <logd25>) . f.(de1950 - <de1950>) . where a, b, c, d, e, f, <logr25>, <t>, <logd25> and <de1950> are constant values given in the table here below for each reference taken into account. The mean bt magnitude is calculated as a weighted mean where the weight (last column) is derived from each source of magnitude as the inverse square of the mean standard deviation. ...

Next: Stellar models Up: Introduction Previous: Photometry Contents . In a hierarchical stellar system, the separation between two neighboring stars is always much smaller than the separation of this pair from the next companion in the system, be it another pair or a single star. ... They are also numerically easier to handle than non-hierarchical systems, since each pair can be described with the standard orbital parameters, and each star with a small number of physical parameters. ... System . ...

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...

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. ...