The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

... The Search of a pulsar Once the dedispersed time series is obtained, a Fourier transformation is performed. ... 2 Binary parameters The orbit of a pulsar , as well as any object, in a binary system is determined in its geometrical characteristics, space displacement and syncronised in time by the following parameters : Semimajor axis Eccentricity Longitude of periastron Binary period Time of ascending node a e PB T0 True spin period and observed spin period The ...

... 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. ...

... Three SCANs were obtained, two were in the -x direction at a wavelengths of 1400 and 2700 and one was in the +y direction at 2700 . ... Models were created to match the GHRS 1400 (FOC F140M filter) and the 2700 (FOC F278M filter) observations, see Figure 38.1 in which model profiles are offset by one pixel. ... The 1400 scan starts to diverge from the FOC model at ~1.0 arcsec, while the 2700 scan tracks the FOC model scan out to a distance of ~1.4 arcsec before diverging from the model scan. ...

... Meta Index / Home Page This section documents the parameters recognized by this task (if any). ... boxhalfsize . yes . ... This should match the value of -boxsize supplied to eboxdetect . ... The cal calculates the truncation point so that the included part of the PSF contains approximately the fraction of total flux specified by the present parameter. ... If psfestyle =`dss', the task looks for the mean energy value in the data subspace of the image set supplied to the present parameter. ...

THE PARAMETERS INVOLVED IN HAPKE'S MODEL FOR ESTIMATION OF THE COMPOSITION OF THE EJECTA LUNAR TERRAINS. ... In the previous papers we were estimated the surface roughness of the ejecta lunar terrains by means comparison of the local phase function and the average integrated lunar indicatrix. ... The Hapke's theoretical model of the lunar surface reflection. ... For THE PARAMETERS INVOLVED IN HAPKE'S MODEL: S.G. Pugacheva, V.V. Shevchenko a low-albedo lunar surface parameter Bo = 1. ...

Irregular phenomena in the Earth Pole oscillation process and temporal variations of geopotential Valery Bondarenko, Vadim Perepelkin s The observed irregular phenomena in the Earth Pole oscillation process are very variety. ... These phenomena indicated in the IERS data are the "abnormal" fluctuation of the Earth Pole coordinates which owing to changing of the geodynamical parameters gives negative result in interpolation and forecast of the first approximation mathematical model. ... Fig. ...

External influences on spin parameters for INTERBALL - AP . ... The main interest is that almost all kind of external influences to parameters of motion (eclipse, normalization, ROS) are presented in the one time interval. Three upper panels illustrate the spin velocity, the angle between kinetic moment and sun direction, and the nutation.All external events are represented on the lowest panel as blue, green and yellow columns. ...

... Column 1 gives the object name from the Case or Markarian catalogs. ... For Markarian galaxies the errors of coordinates usually lie inside 2'' (Lipovetsky [ 1983 ]). Column 4 gives the eye-estimated apparent blue magnitudes according to the same sources. ... Other names of a galaxy we give in column 7. ... In column 3 we cite the original emission-line code of the galaxy for the strength of [O III ] doublet according to the Case catalog (s - strong, m - medium, w - weak). ...

... Several of the tasks in the spectral package share a common set of parameters. ... Each task in the spectral package has a hidden parameter which points to the pkgpars parameter file. The parameters stored here include the observed data sets and the model descriptor, and instrument-specific parameters. ... The observed counts and error data set contained in the table file ( *_obs.tab ) produced by qpspec will be the input data for subsequent spectral tasks. ...

Next: Date conversion functions Up: Command line procedures Previous: Analysis procedures Contents . list_names [, names _char ] List HDS objects at current level. Store in parameter, if given. list_tree List HDS tree beginning at current level. list_scans [, index ] List observed scans, stars, times, stations, and codes. If index is specified, list only these scan IDs. list_bgscans List stars and back ground scans. list_stars [, stars _char ] List stars present in currently loaded data. ...

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. ...

SPECTRUM ANALYZER OF MAGNETIC PHENOMENA SAMW . Spectrum analyzer allows onboard computation of electromagnetic waves spectra registered (observed) in the ionosphere and magnetosphere in the ELF/VLF frequency band. ... It consists of magnetic antenna, preamplifier, 16 bit sigma delta AD converter, DSP processor and telemetry interface. ... The channels of lower frequencies are averaged and transmitted with lower repetition rate so the telemetry volume is reduced. ... Dynamic range: 90 dB . ...

MINUTES of the RadioAstron Teleconference on December 13, 2011 Yu.Yu. ... IOC status update M. Popov informed the participants on the current IOC results. ... Kovalev added: we continue to observe pulsars and spectral line sources in radiointerferometer mode but only with spacecraft and we are also going to observing pulsars soon with space-ground baselines. ... Kovalev: It is fringe-fitting result. ... In RAFS05 we replace it with K-band observing (maser source Ori KL ­ spectral lines ~100000Jy). ...

... Duchamp | ... Top | Duchamp is a solution to this problem of three-dimensional source finding. ... A list of the detections and their properties, as well as the input parameters that were used. [text file] . ... It can be downloaded in source format, in a gzipped tar archive. ... Changes from the previous version can be seen here (this file is included in the tar archive), while the archive files and documentation from the previous release versions are here , if you are really interested. ...

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... Investigations of the ionospheric response to strong magnetics storms which are usual for our latitudes, are of great interest. ... In the figure, we present ionospheric parameter dynamics during three perturbed days in July 2000. ...

... There is an opportunity to perform O-C calculations for objects which are absent in the data base of the package. Such objects can be described by orbital elements or by initial coordinates and velocities. ... On pressing Edit file button user has a possibility to look through the list of object elements or their coordinates and velocities to add or to change it. ... For example, the designations of objects in the list can occupy the last position in each line. ...

... Contacts . 2012: . ... We refined the fundamental parameters of the components, the orbital periods, and the conditions of photospheric heating of the secondary component by the ultraviolet radiation of the hot component. ... The observations of the star clusters associated with ultra-luminous x-ray sources (ULXs) in four galaxies on the 6-meter and VLT telescopes have shown that all the ULXs are located within 200pc of very young star clusters (younger than 5 million years). ... Archive . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Top panel: comparison between the observed H and H line profile (black solid line) and synthetic profiles calculated with the final adopted parameters (dash-dotted green line) and with the parameters which were found to best fit the hydrogen line profiles (dashed red line). ... We provide photometric and spectroscopic evidence showing the star is most likely a member of the young Stock 16 open cluster (age 3тАУ8 Myr). ...