... Format of the orbital elements | Estimation of the extrapolation errors | Version 1" of the orbital elements collection, determined by KIAM during flight and used for operations planning . Version 2" of the of the orbital elements collection, modified by IKI during flight and recommended for the orbital calculations during scientific data processing . ... Three kinds of the INTERBALL Auroral probe (IB_AUR) orbital elements' collections are presented here. ... IKI RAN | SSC IKI RAN | ...

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• STDA files
• About modification of the INTERBALL orbital elements
• The INTERBALL Tail PROBE orbital elements

... User Guide ] Task: moment Purpose: Calculate moments of a Miriad image. ... Key: in The input image. No default. ... Key: mom -3: Velocity at peak intensity using a three-point quadratic fit around the peak (km/s). 2: Peak intensity using a three-point quadratic fit (units same as individual channels). ... The moments are calculated independently for each pixel using spectral channels with intensity satisfying the specified clip range. ... Key: axis Axis for which the moment is calculated. ...

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• selfcal
• uvfmeas
• gpdof

. This diagram shows a small table with three transparent cells and illustrates how their final background is determined. The table consists of two rows. Four (labeled) cells lie in the first row, but the second cell spans the first and second row. The first, third, and fourth cells of the second row are "empty". Each non-empty cell has a red background and a double black border. Each empty cell has the table's background color (specified as #ff0) as its own. Return to image.

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• Long description of example illustrating table row height calculations and

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• THE HUBBLE LAW JAVA APPLET
• Redshift Tutorial

Next: Discussion Up: The Second EGRET Catalog Previous: First Catalog Sources . In the first EGRET catalog, upper limits were given for selected objects not detected during the Phase 1 all-sky survey. These upper limits are determined using the likelihood calculation and depend on the EGRET exposure to a given direction, the contribution of the diffuse gamma radiation, and the proximity and strength of detected sources. ...

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• Catalog Construction
• Flux Calibration and Extinction Correction

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

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... The evolution of a binary system is considered as a sequence of stages the duration of which are defined by the shortest evolutionary time-scale of one of the binary components (see the list of the evolutionary states of stars in Sections 3 and 4). ... Then the code finds a new stage the binary should transit to, with this stage being determined by the evolutionary states of both components, and calculates it. ... However, one can use the algorithm described above to model their evolution. ...

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• Change of Binary Parameters: Mass, Semi-major Axis and Eccentricity
• Introduction
• Notes on Monte-Carlo Simulations

... The absolute flux calibration of NICMOS will be calculated from observations of standard stars with known flux distributions F( ). ... In order to expand the set of IR standard stars in the appropriate flux range for NICMOS, M. Rieke, R. Thompson, and collaborators at the University of Arizona are making photometric observations of solar-analog stars, which will be used to normalize the solar spectrum to the observed IR magnitudes. ... Relative flux references accurate to 1.5% for standard...

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• The Flux Ratio Method for Determining the Dust Attenuation of Starburst...
• How do I best determine an observation's actual orientation?
• ALUMINUM SUPERCONDUCTING HOT-ELECTRON BOLOMETER MIXERS FOR THz APPLICATIONS -

THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE BY MEANS OF DIGITAL MODELS. ... The surface brightness of Mercury was measured Danjon (1933, 1949, 1953) and Harris (1961) in phase angle 3o-123o. The analysis of the various data of the integral photometric gives the results of determination of the main photometric constants for Mercury. ... THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE: S.G. Pugacheva The surface brightness of the Mercurian images was established on the geologic map Mercury. ...

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• http://selena.sai.msu.ru/Ber/Publications/ms40/88_Yamashita%20et_al.pdf

Triad, launched September 2, 1972, was an experimental spacecraft designed to move in an accurately predictable low-altitude orbit, allowing its position to be used as a reference point in navigation. ... While the "proof mass" thus moved in an accurately predictable orbit, the spacecraft itself was subject to air resistance and sunlight pressure, causing it to move slightly differently. ... Exploration" home page (index) Glossary . Official GSFC Home Page .. NASA WWW Home Page . ...

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... ON THE ROLE OF LARGE-SCALE PLASMA IRREGULARITIES AT THE FINAL STAGE OF ANOMALOUS ABSOPTION DEVELOPING UNDER HF HEATING OF THE IONOSPHERE . ... Fig. ... With the aid of numerical statistical modeling based on multiple ray tracing it is shown that in presence of large-scale irregularities the reflected signal amplitude mean value is increased significantly. ... Dependence of the mean amplitude of the reflected from the ionosphere signal on the large-scale (10-50 km) electron density irregularity level...

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• MONTE-CARLO
• POWER SPECTRUM OF THE IRREGULARITIES AND IT'S FIXING
• Anomalous Absorption Theory

... 8, ``Celestial Mechanics'', 2002 An approximate projection of confidence ellipsoids of space objects positions onto the celestial sphere A. P. Baturin Research Institute of Applied Mathematics and Mechanics, Tomsk, Russia The approximate method of calculation of a visible border of probable motion regions (PMR) for space objects (SO) has been considered. ... As a result, the simple analytical expressions for border points of PMR projection onto the celestial sphere have been obtained. ...

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• Values of asteroid masses
• (Untitled)
• ENGAMPLE

... 2006: . ... Components of the systems are low mass stars and white dwarfs. For 14 pairs orbit parameters were calculated and masses and luminosities of components were determined for the first time. ... As a result of a multifrequency monitoring of the variability of a micro quasar Cyg X-3 (X-ray binary system which probably consists of a black hole and a high mass Wolf-Rayet star) a high activity period was registered for the first time in the last 4 years. ... Archive . ...

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• IRAS01005+7910
• topic_en

Institute of Applied Astronomy Russian Academy of Sciences Method of Determining the Orbits of the Small Bodies in the Solar System Based on an Exhaustive Search of Orbital Planes Dmitrii Vavilov, Yurii Medvedev Introduction to the problem: Let we have n 3 positional observations of a body: points in time ( = 1, ) , right ascensions , and declinations . ... Determination of the orbit using the Gauss method of determining orbital elements based on two heliocentric positions and points in time. ...

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Halley's Comet . Spacecraft that have visited Halley's Comet . ... Then in 1984 and 1985, five spacecraft from the USSR, Japan and Europe were launched to make a rendezvous with Halley's Comet in 1986. ... This image is a mosaic of 8 images taken by the Giotto spacecraft during the Halley encounter on March 13, 1986. ... Courtesy NASA/JPL) . ... Halley's Comets in 1986 . This image of Halley's Comets was taken during its 1986 appearance. ... Cylindrical Map of the Nucleus of Comet Halley . ...

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• The Arcetri Spectral Code file format
• CHIANTI atomic database
• IBIS - Flat Fielding

Next: Infrared Data Up: Contents Previous: Optical Photometry . ... For example, one method is to derive the spectral energy distribution (SED) for a target star and compare it to the SED of a dereddened standard star. ... Temperature can be determine via the B - V color (Gilliland 1985): . ... The results produced small extinctions to the background stars of between A and A . ... The most accurate extinction calculation requires both IR and spectral data. Infrared Data . Spectroscopic Data . ...

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• *imcnts* - Azimuthal profile of an extended source
• Stars with Less Secure Periods
• Fits to Evolutionary Models

Next: DIRECT MASSES FOR BXCIR Up: EXTREME HELIUM STARS: PULSATION Previous: PULSATION PROPERTIES . As already indicated, V652Her is an important EHe star because its relatively short pulsation period and large amplitude pulsations allow its overall dimensions to be determined with high precision. ... Saio & Nomoto (1998) made the first successful models for the merger of two carbon-oxygen white dwarfs, and prompted Saio & Jeffery (2000) to attempt models for the merger of two helium white dwarfs. ...

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• Armagh Observatory
• A Statistical Study of the Relationship between the Solar Cycle Length and
• Abstract

... When creating a mosaic from a set of individual frames, the correct background offset for each frame must be determined for proper matching. In this paper we describe a method for constructing a mosaic from a set of individual frames by applying a minimization technique. ... Typically these are frames with some known defect (see ? ... Determining which frames to exclude from the final mosaic is critical, since one bad frame can create background offset errors that propagate throughout the mosaic. ...

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• Calculating the Position and Velocity Components of HST
• A Technique for Determining Proper Motions from Schmidt Plate Scans at ST ScI
• NICMOS Calibration Pipeline: Processing Associations of Exposures

. XMM-Newton Science Analysis System . slconv (slconv-2.1.3) [xmmsas_20070708_1801-7.1.0] . Meta Index / Home Page / Description . Several region shapes can be selected through parameter shape : circle, box, diamond, ellipse and boxcircle. The size of these regions is determined once the radii is calculated as explained in previous section: . - box side = circle_radius . - ellipse_minor_axis= circle_radius . - ellipse_major_axis= circle_radius . XMM-Newton SOC/SSC -- 2007-07-08

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• The contour method of calculating source region shape

... Shortly after its discovery it was determined to be in a highly elliptical path near Jupiter and on a collision course. ... The size and mass of the original body and the individual fragments is as of this writing still highly uncertain. ... Between 16 July 1994 and 22 July 1994 the fragments impacted the upper atmosphere of Jupiter. ... The pictures were posted to the Net within hours of the impacts and caused severe overloading on some ftp and WWW sites. ... JPL's SL9 page . ... Small Bodies .. ...

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• NIST Modem Time Service
• authspeed - determine authentication delays
• NASA determines supernova remnants create cosmic rays