... Broadening is due both to the natural width of the transition and to the velocity spread of the absorbing atoms along the line of sight. In the ideal case of atoms at rest. ... In the program the velocity is assumed to be gaussian, thus: . velocity of the cloud relative to the observer. ... An absorption is measured in the spectrum at = corresponding to a rest wavelength . ... In practice the program computes the absorption profile in the cloud reference frame . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Lower panel: The ME spot map of the star in orthographic projection, showing the disc of the star as it would be seen by an observer on the Earth at the labelled rotation phases (see the text). ... We carried out high-resolution spectroscopy and BV(I)C photometric monitoring of the two fastest late-type rotators in the nearby Pictoris moving group, HD 199143 (F7V) and CDтИТ64 1208 (K7V). ...

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. ...

http ://hea-www.harvard.edu/ AstroStat /slog/2008/eotw-chisq- distribution / Weaving together Astronomy+Statistics+Computer Science+Engineering+Intrumentation, far beyond the growing borders Fri, 01 Jun 2012 18:47:52 +0000 hourly 1 http ://wordpress.org/?v=3.4 http ://hea-www.harvard.edu/ AstroStat /slog/2008/eotw-chisq- distribution /comment-page-1/#comment-308 Alex Sun, 27 Jul 2008 01:52:08 +0000 http ://hea-www.harvard.edu/ ... Thanks, Aneta, very useful comment. ...

... The Network Time Protocol (NTP) is used to synchronize the time of a computer client or server to another server or reference time source, such as a radio or satellite receiver or modem. ... Information on the NTP architecture, protocol and algorithms can be found in the Further Information and Bibliography page. The Building and Installing the Distribution page presents an overview of the procedures for compiling the distribution and installing it on a typical client or server. ...

... 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...

spaceweb@oulu.fi - last update: 28 May 1995, 0800 UT . Advanced plasma theories are extremely important when one tries to explain, for example, the various waves and instabilities found in the plasma environment. ... In the kinetic theory it is necessary to know only the distribution function for the system of particles. ... The dependence of the distribution function on the independent variables r , v , and t is governed by an equation known as the Boltzmann equation . ... Hot plasma theory . ...

... Abstract Return the relative difference between two vectors of general dimension. Required_Reading None. ... Detailed_Input v1, v2 are two vectors for which the relative difference is to be computed. ndim is the dimension of v1 and v2. Detailed_Output vrelg_c is the relative difference between v1 and v2. ... Particulars This function computes the relative difference between two vectors of general dimension as defined above. ... Index_Entries relative difference of n-dimensional vectors . ...

... We are using Canadian Galactic Plane Survey l 74.2њ, -3.6њ < b This poster gives preliminary results for a full-fledged analysis of the gas properties and distribution of HISA features in the CGPS. ... where T ON and T OFF are observed brightnesses on and off the HISA feature, T S is the spin or excitation temperature of the HISA gas, tau is its optical depth, T C is the continuum intensity, and p is the fraction of H I emission lying behind the HISA feature. ... GIF | ...

Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

... The following algorithm shows the rough details of these calculations. ... Similarly the energy selection region for the reflection order of the output matrix is converted to the array called banana. // analyze the exposure maps within the spatial selection regions FOREACH node FOREACH b = dispersion channel of node src.exposure[ node ,b] = EXPMAP node [b] summed over src.spans[ node ,b] bkg.exposure[ node ,b] = EXPMAP node [b] summed over bkg.spans[ node ,b] D = EXPMAP ...

... Here we present our first results of a study of the neutral hydrogen gas (HI) in the southern spiral galaxy NGC 253 with the Australia Telescope Compact Array . ... Several peculiar features have been found. ... Similar features have been found in other starburst galaxies like M82, NGC 1808 and NGC 4945 and are interpreted in terms of bar-induced gas dynamics and star formation. Keywords. galaxies: individual (NGC 253) - galaxies: active - galaxies: ISM - galaxies: kinematics and dynamics. ...

... From the uvby photometry and proper motions for about 5500 nearby F stars we have found the following: (i) F stars , taken in narrow ranges of metallicity , show at [fe/H] 0 rather distinct cut-off in their distribution along the Main Sequence (MS) at the blue side, which is suggested to be an indication for the MS turn-off in stellar groups of fixed metallicity ; (ii) the corresponding turn-off age from theoretical isohrones strongly correlates with the ...

... Subject and Problems of Stellar Astronomy. ... Plane of Galaxy, Methods of Its Location Determination. ... Stars Distances. ... Other Methods of Stars Distances Determination. ... Tangential Velocities, Their Determination by Self-Motions. ... Determination of Solar Apex and Spatial Velocity by Radial and Spatial Velocities of Stars. ... Features of Orientation and Parameters of Peculiar Stellar Velocities Ellipsoid. ... General and Selective Light Absorption in Galaxy. ... Darc Clouds in Galaxy. ...

... Results 3. ... 2004), Escapa (2011): Hamiltonian approach, simplified elastic response. ... PАg. ... Let us recall that assuming a rheological model based in Smith (1974) , Wahr (1979) and IERS (2010) for the elastic/anelastic response of the Earth, the second order harmonic components of the redistribution potential admit a truncated development in complex spherical harmonics in the form Generalized Love Numbers, dependent on: Harmonic order, Excitation frequencies In magnitude, PАg. ...

... Spectral energy distributions (SEDs) for active galactic nuclei (AGN) are made publicly available by computing self-consistent 2-phase AGN torus models. ... Dust extends from the dust evaporation radius, typically located between pc/10 Heymann Siebenmorgen (2012). We consider fluffy dust particles ( Kr gel Siebenmorgen , 1994). ... As an example we show below the SEDs of an AGN computed with diffuse ISM dust ( Siebenmorgen et al 2014) and fluffy grains ( Kr gel Siebenmorgen 1994) . ...

... This will be done by fitting period-luminosity relations in the form V = a в log P + b to Cepheid variables in these two galaxies. ... 8 Marks 2. ... 3R x3 2 Marks (b) Use this expression for the pressure to show that when 1 is constant, the adiabatic wave equation for the star can be written as x d d 3 R3 2 3 [(x - x4 ) ] + [ x - (31 - 4)] = 0. dx dx 1 GM 2 Marks (c) Show that near x = 0, the solution to this equation is of the form = Ax , where A is a constant and 2 = 3 (31 - 4). ...

alignasn -- Change the relative shifts in association file alignasn association . ... calnicb style association file with list of images to be aligned. ... Interactive program to compute relative shifts of images in an association file. ... After computing the relative shifts of the direct images, alignasn searches for corresponding grism images for each of the direct images. ... The grism association is then updated with the same relative shift measurements as determined from the direct images. ...

Measuring system: (1) is alternating voltage source, connected to transmitting electrode, (2) is phase sensitive voltmeter, connected to receiving electrode, (3) is grounded shield, (4) is object under imaging, (5) is unperturbed electric field lines connecting transmitting and receiving electrodes. ...