ASC-FITS-2.0.1: ASC FITS File Designers' Guide (Rots and McDowell) (1999 Jun) . ASC-FITS-REGION-1.0: FITS region document (McDowell and Rots) (1998 Mar) . ... CXC-DM-001 Introduction: Data Analysis with the Chandra Data Model (2001 Oct) . ... 1998 Feb 26: SDS-1.0: Data Product List: obsolete . ... 1998 Mar 09: SDS-10.0: (ASC-FITS-REGION-1.0) FITS region document: see ASC-FITS-REGION-1.0 . 1998 Feb 09: SDS-11.0: FITS function document (superseded by ASC-FITS-FUNCTION-1.2) . ...

... The most powerful and widely used methods to calculate the scattering matrix of a fractal cluster are based on the coupled dipoles methods (e.g. the Discrete Dipole Approximation, DDA) and the theory of light scattering by a cluster of spherical particles [2-4]. ... At present the procedure of calculation of the scattering matrix is well developed for both an oriented cluster of spherical particles and for chaotically oriented clusters of such particles [4]. ...

... 2001 July 10 . Sudbury Indicates Nonstandard Particle Model . ... The Sudbury Neutrino Observatory Institute . Explanation: The Sudbury Neutrino Observatory (SNO) has been detecting so few neutrinos from the Sun that the Standard Model of fundamental particles in the universe may have to be revised. Pictured above is the SNO as it was being built. ... The most popular model for fundamental particles , known as the Standard Model , did not predict such schizophrenic neutrinos . ...

Astronomy Picture of the Day . ... The Sudbury Neutrino Observatory Institute Explanation: The Sudbury Neutrino Observatory (SNO) has been detecting so few neutrinos from the Sun that the Standard Model of fundamental particles in the universe may have to be revised. Pictured above is the SNO as it was being built. ... The most popular model for fundamental particles , known as the Standard Model , did not predict such schizophrenic neutrinos . ... The Sudbury Neutrino Detector . ...

The Earth's magnetosphere global structure is conditioned by the interaction of the Solar wind and Earth's magnetic field. ... Solar wind (SW) - the region outside BS; . ... Auroral field lines (AUR) region - the funnel-shape cavity restricted by the geocentric distance of the order of 6 RE, between surfaces formed by magnetic field lines emerged from the polar and equatorial OVAL borders; . ... Fairfield D.H., Average and unusual location of the Earth's magnetopause and bow shock, J. Geophys. ...

... The magnetic field of the Earth has been investigated by satellites for several decades now, and enough of it is known to model its average strength and shape during different levels of overall magnetic activity. Presently the most used empirical global magnetic field models are the Tsyganenko models (1987, 1989) , referred to as T87 and T89, respectively, although even these consist of several submodels. ... Earth's magnetic field from T89c model during Kp=2 for different seasons. ... Res. ...

... Modelling is the only feasible way of assessing the reliability of the reconstructions. Modelling here refers to the model used to generate a simulated data set, not the implicit modelling performed by the deconvolution algorithms.) ... Model-fit for parameters to the original data if possible. Check that simulated observations can recover the significant features of the model reliably. ... Use simulated observations to determine the effective resolution of the deconvolution sky model. ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... Australia Telescope 20GHz Survey . ... Visiting Parkes radio telescope . ... Parkes radio telescope webcam . ... Probing ISM Models with H observations . ... Turbulent Models of the ISM . ...

The Steady State model of the Universe was proposed in 1948 by Bondi and Gold and by Hoyle. ... At the time the Steady State model was proposed, the Big Bang model was in trouble because the value of the Hubble constant was clearly bigger than the inverse of the age of the Universe. ... Thus the Steady State model has flat spatial sections like the critical density Big Bang model. ... The Steady State model has no adjustable parameters to correct for this error, but the Big Bang does. ...

... 2.3 Establishing the Extragalactic Distance Scale . ... 2.3.2 The Second Rung: Distances to stellar clusters . ... 2.3.4 Distances to Local Group Galaxies . ... The Luminosity Function of Planetary Nebulae . ... 3.2.2 Clusters of Galaxies . ... 4.2 Evidence for Dark Matter as a Function of Scale Size . ... 4.3 Other Dark Matter Indicators for Galaxies . ... What is the nature of the large-scale distribution of matter in the universe as traced by the three-dimensional galaxy distribution? ...

Gerry Doyle's homepage . Watch this space!

. Language [RU/EN] Search: . Home . UP . Research . Projects . Services . Info . News . Events . Personal . Archive . Ionosphere . Ionosounding: . PARUS . Digisonde . Data: . Moscow . St.Petersburg, Kaliningrad . Models: . SM-MIT . --------------------------- . Forecast . Ionospheric weather . Structure . Contacts . N.V. Pushkov . 10/04/2016 01:10 MSK . webmaster@izmiran.ru . Click on the image above to open SMF2 model page . (C) 2007, IZMIRAN

... Science Activities > PhD Thesis Topics offered by ESO Faculty Members > Thesis Topic: Dynamical models of multiple globular cluster populations around massive galaxies . ... Different techniques have been devised to separate multiple GC populations and perform dynamical analyses. ... Within this project, the PhD candidate will examine mock models of multiple GC populations around massive galaxies, devising `blinded' functional tests and comparing the possible sources of bias in different techniques....

... Bojan Nikolic web pages home . ... As an exercise to put through the new InMin library through its paces, I have looked recently at applying Nested Sampling ( Skilling2006 ) algorithm to the fitting of star-formation history as function of redshift. ... The data I used are from Figure 1 of Yuksel08 but I use only the grey data paints, which are just the data originally from Hopkins2006 . ... The next step is to define the function which is the model for the history of the SFR density. ...

... Next: Cheating Poisson: A Up: Statistical Analysis Previous: Spatial Models and . ... The spatial distribution of stars in the Local Group dwarf irregular galaxy NGC 6822 has been studied, using recent positions and deep photometry for about 15,000 stars in the galaxy. Based on photometrical data, OB stars and red stars could be studied separately. Spatial statistical tools have been applied to the analysis of the spatial structure. ... Figure: Model selection by the aid of CAIC . ...

Cost Estimating Web Site . ... 2005 NASA Cost Analysis Symposium Databases . ... World , European Communities , Other European Countries , Americas , Asia , Africa , General US , US Federal Government , US Department of Defense , Aerospace Industry , NASA , Science & Engineering Handbooks . NASA Cost Estimating Handbook 2004 , Parametric Estimating Handbook .. ... Consumer Price Index , Employment Cost Index , GDP Deflator , Import Price Index , NASA New Start Index , Producer Price Index . ...

MATHEMATICAL MODELING: . ... This model is developed on the base of the probabilistic description of the collisional aeronomical processes and is realized on a computer as the numerical system (stochastic model). ... Shematovich, V.I., Bisikalo , D.V.             Nonequilibrium processes in the planetary and cometary atmospheres. ... In Russian) . ... Piarnpuu , A. A.; and Shematovich, V. I.       Construction of structural stochastic models of collision processes in rarefied gas media (abstract) . ...

... Comparing the periods from the model and P2030 data (.ps) ( .pdf ) . aeroPer.dat...file containing aerostat periods. ... The model was then used to determine the periods that it could generate in pulsar observations. ... rf pulse length: 320 Useconds (this is actually 2 160 usecond pulses that are sequential in time). 7 ipps of 3771., 3504., 3076, 2809., 2903.5, 3289., and 3676. useconds. blanking of the radar signal for 42 degrees of azimuth centered on the observatory direction. ...

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