... If the hydrogen content x is low and the interaction among the H atoms is negligibly small, the total scattering intensity S can be written as: S = xSH + (1 - x)S PdD Pd D arb. units x 1{ x Hx = 0 .0 5 0 0 .0 7 2 0 .0 9 1 S(Q, !), 0 40 80 !, meV 120 160 200 Fig. ... 2 2 2 X U (K ) Ў L Ў The calculated g ( ) spectra of the PdD1-x Hx solutions cannot be directly compared with their experimental S (Q, ) spectra because of the significantly different cross-sections for neutron scattering by H and D...

These are very prominent absorption lines is most all galaxies. ... These pair of absorption lines will appear in all the spectra and they should be your principle source for determining the redshift. ... When this applet opens you will see an iconic representation of galaxies in the left hand side of the applet and a target area in the right side of the applet. ... Note: What you are doing in this excercise is identical to what Hubble did in the 1920's and you are using the same galaxies. ...

Detector of hydrogen isotopes (ISIV) . ... Measurements of hydrogen isotopes content in surface layer of a solid (provided that the content is more than 0.01 %). ... Content of hydrogen isotopes of a sample is measured by nondestructive technique of direct measurements in the surface layer. ... Measurable hydrogen isotopes content   ~0.01 wt. ... Area surface of sample                                         ~10 cm 2 . ... G. Dolnikov +7(495)333-25-66, ggd@iki.rssi.ru . ...

Next: Model of clusters Up: paper2 Previous: paper2 . ... It allows estimating different microphysical properties of scatterers (size, complex refractive index, shape, etc.) from measured characteristics of the scattered radiation. ... The complexity of the direct problem depends on its input parameters characterizing the shape, size and structure of the scattering particle. ... Next: Model of clusters Up: paper2 Previous: paper2 root 2003-04-11 ...

... Files . ... measures . ... appropriate 'set' 00115 // methods 00116 ParAngleMachine (); 00117 // Construct for the specified direction 00118 ParAngleMachine ( const MDirection in); 00119 // Copy constructor (deep copy) 00120 ParAngleMachine ( const ParAngleMachine other); 00121 // Copy assignments (deep copy) 00122 ParAngleMachine operator= ( const ParAngleMachine other); 00123 00124 //# Destructor 00125 ~ParAngleMachine (); 00126 00127 //# Operators 00128 // Return parallactic ...

... To serve as an example, the first is laid out below. subroutine calcSpatial00(ccd, node, imageModel, etc) # startEbin = first Ebin with centre energy greater than TS minimum E. # stopEbin = last Ebin with centre energy less than TS maximum E. numerator = 0.0 denominator = 0.0 if (imageModel eq 'point') { # eqn 33, 34 of SSC-LUX-TN-0053 foreach Ebin (startEbin .. stopEbin) { call CAL_getPSFmap(PSFmap) expr = 0.0 ...

We measured the spectrum of polarization for three proto-planetary nebulae (PPNs), IRAS 17411-2411, IRAS 08005-2356, and IRAS 04296+3429, and made model calculations with the dust-scattering Monte Carlo code DIRTY and the dust emission code 2Dust. ... Modeling the spectropolarimetry of IRAS 04296+3429 indicates a point-symmetric, multipolar morphology in the PPN phase. ... ADS Citation Query . citations = 11 . citations vs. year [year,citations] . ...

... We have measured this "redshift" for the pink black holes, and allowed for it in our calculations. ... We see this effect in the emission from gas around these pink black holes, but it is far too small an effect to account for the pinkness. Thus the swirling motions of gas around or into the black holes cannot produc the colour. ... At first we thought that these things were normal blue black holes hidden behind clouds of interstellar dust, that absorbed the blue light and made them appear pink. ...

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

Microsymposium 40, abstract 88, 2004 (A4 format) GAMMA RAYS FROM MAJOR ELEMENTS BY THERMAL NEUTRON CAPTURE REACTIONS: EXPERIMENT AND SIMULATION FOR PLANETARY GAMMA-RAY SPECTROSCOPY. ... Then the calculation can be restarted by producing gamma rays and let them trans- GAMMA RAYS FROM MAJOR ELEMENTS BY THERMAL NEUTRON CAPTURE REACTIONS: N. Yamashita et al. port and react, with initial energies determined the outside multiplication and initial locations wh neutron capture reaction took place. ...

... Archives . ... Magnitude [Eqn] . ... Differential Emission Measures (DEMs) are a summary of the temperature structure of the outer atmospheres (aka coronae) of stars, and are usually derived from a select subset of line fluxes. ... is called the Differential Emission Measure and is a very useful summary of the temperature structure of stellar coronae. ... Tags: DEM , Differential Emission Measure , EotW , Equation , Equation of the Week , stellar coronae . ... Comment ( RSS ) | ... Chandra Blog . ...

... Previous: Background Fluctuation Analysis from the Multiscale Entropy . ... A new measure of information is defined which is based on noise modeling and incorporates resolution scale. Properties of this measure are discussed. ... Additionally it allows for image noise modeling, and subsequent noise removal. ... Hence information- and entropy-based processing technologies will be necessary for the effective design and implementation of large, future generation, image databases. ...

... A comparison of the computed and experimental relations F max ( H), as well as comparison of drift scans of point sources across different horizontal cross-sections of the BP with the corresponding computed cross-sections were made. ... The drift scans of the point source 3С84 (H=87 o ) at the wavelength 7.6 cm across the horizontal cross-sections of the BP (black lines) and the computed horizontal cross-sections of the BP corresponding to them (red lines). ...

This section is on a higher level than the rest, and is primarily meant for advanced users, who may wonder how orbital motion is actually derived. ... As stated earlier, the motion of a satellite (or of a planet) in its elliptical orbit is given by 3 "orbital elements": . ... 3) The mean anomaly M , an angle growing at a steady rate, increasing by 360 degrees each orbit . ... In polar coordinates ( r,f ) describing the satellite's motion in its orbital plane, f is the polar angle. ... The angles: . ...

SLIDE 1 Coherent beam­beam e#ects study. ... He has shown that a finite length (in other words equal to # # ) of colliding bunches can lead to the coupling of synchro­betatron modes in the beam­beam system, and thus a head­tail type instability of colliding bunches may arise. ... These modes have been observed in di#erent machines. ... SLIDE 5 Figure shows the dependence of the measured and calculated synchro­betatron mode tunes on the beam current for equal electron and positron bunch intensities. ...

... DIAGNOSTICS OF IONOSPHERIC IRREGULARITY SPECTRUM USING MEASUREMENTS OF RADIO WAVE ANOMALOUS ATTENUATION UNDER VERTICAL SOUNDING . ... The selected experimental data are characterized by a high average level of attenuation of a signal of vertical sounding (10 dB and above), which cannot be caused by collisional absorption of radio waves (practically absent in a dark time of day) and, hence, being a consequence of scattering on random irregularities. ... ATTENUATION OF A VERTICAL SOUNDING SIGNAL . ...

Next: Pulsations Up: PHYSICAL CHARACTERISTICS Previous: PHYSICAL CHARACTERISTICS . The fundamental properties of RCBs may be deduced from their spectra at maximum light. ... The properties of a stellar atmosphere may be measured from both the large-scale features - the broad-band flux distribution - and the detailed spectrum of absorption lines. ... They show that, in general, hydrogen makes up less than one part per thousand down to less than one part per million of the stellar atmosphere. ...

Application of X-ray Crystallographic Detector to Whole Breast Digital Mammography . ... Our system is composed of modules in which a gadolinium oxysulfide phosphor is deposited directly onto a fiber optic taper which is bonded to a CCD. ... We present measured MTF and light output data from Gd2O2S:Tb phosphors of various thicknesses, and discuss implications for the developmental breast imaging detector. ... The measured module MTF is significantly poorer than that of its phosphor alone (Figure 1). ...

Magnification (Power) And Using Eyepieces . ... To determine power in a telescope, divide the focal length of the telescope by the focal length of the eyepiece. By exchanging an eyepiece of one focal length for another, you can increase or decrease the power of the telescope. For example, a 25mm eyepiece used on a telescope with a 1000mm focal length would yield a power of 40x (1000 / 25 = 40) and a 10mm eyepiece used on the same telescope would yield a power of 100x (1000 / 10 = 100). ...

Plot of Pulse broadening time at 1 GHz vs. dispersion measure DM for 196 pulsars. ... A similar plot with fewer pulsars appears in Nature , 354 , 121, 1991 (Cordes, Weisberg, Frail, Spangler & Ryan). ... Dynamic Spectra from Pulsar B1919+21 in 1980-1981. These data obtained at the Arecibo Observatory were reported by Cordes, Weisberg & Boriakoff 1985, ApJ , 288 , 221 and Cordes 1986, ApJ , 311 , 183. Dynamic Spectra from Pulsar B0329+54. ... Dynamic Spectra from Pulsar B1933+16. ...