. Proceedings of Turbulent Shear Flows XI, Sept. 1997. Jacques Lewalle, jlewalle@syr.edu

... As sketched in Fig. 3, registered images are influenced by fractions of the original signal from outside the domain of measured data. ... Inner Region . ... A rigorous solution which completely avoids the boundary problem is the extension of the region of restoration by the extent of the point spread function. If the extent of the measured data is 512 512 and the extent of the point spread function is 256 256, the extent of the region of the restoration should be (512 + 256) (512 + 256) = 768 768. ...

Next: Blinkers and Bi-directional Jets Up: J.G. Doyle, Research Astronomer Previous: J.G. Doyle, Research Astronomer . Gerry Doyle reports that collaborative research with Maria Madjarska has revealed for the first time the presence of bi-directional jets and magnetic reconnection occurring at coronal hole boundaries. ... Next: Blinkers and Bi-directional Jets Up: J.G. Doyle, Research Astronomer Previous: J.G. Doyle, Research Astronomer M.E. Bailey . ...

. unfiltered . PC 1 secular . Difference between last and first map of PC1 . PC 1+2 annual . PC 2 . PC 3 . PC 4 . PC 5 . Sum of nine first PC's 2-10 . Difference between the initial signal and ten first PC 1-10 .

... Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Field Field designation (1) 10- 11 I2 h RA1h First boundary field right ascension ( 1950.0 ) 13- 14 I2 min RA1m First boundary field right ascension ( 1950.0 ) 16- 20 F5.2 s RA1s First boundary field right ascension ( 1950.0 ) 22- 23 I2 h RA2h Second boundary ...

Growth of Epitaxial (001) YBa2Cu3O7 Superconducting Thin Films on (001) Diamond Substrate. ... In order to reach higher frequencies and lower losses, it is necessary to use substrate material with lower dielectric constants and low losses in far infrared region. ... In the present work, as a first step in this direction, we present results of successful growth of epitaxial (001)YBa2Cu3O7 thin film on (100) diamond substrate by pulse laser deposition method. ...

ON THE IMPACT OF THE GALACTIC ABERRATION ON VLBI-DERIVED PRECESSION MODEL Z.M. MALKIN Pulkovo Observatory Pulkovskoe Ch. ... Corrections to adopted precession rate are usually computed from the linear trends in long-term time series of celestial pole offset (CPO), which are the differences between the measured and the theoretical coordinates of the celestial pole. ... CONCLUSIONS We have estimated the impact of GA on parameters of precession-nutation model derived from VLBI observations. ...

... Moscow, Russia E-mail: krivosheev@iki.rssi.ru Notes: · · The Monte Carlo method (s) is also called the statistical test method An innumerable number of processes can be listed the outcome of which is not determined and has probabilistic nature, but these processes obey statistical laws, so to obtain the result we have to make multiple similar tests, i.e. to use the MC method Because probabilistic processes are widely spread in nature, the MC ...

... Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Kamogata, Okayama 719-02, Japan, E-mail: yoshida@oao.nao.ac.jp . The Mitaka-Okayama-Kiso data Archival system second version (MOKA2) has been released. ... Is was developed for the observational data taken with the Spectro-Nebulagraph (SNG; Kosugi et al. 1995) attached to the 188cm telescope at Okayama Astrophysical Observatory and with the prime focus CCD camera of the 105cm Schmidt telescope at Kiso Observatory. ...

... Use the ROSAT broad band background which is a array file at 1/30 the *.qp file resolution, and contains data from PI bins 7-240. input files: xdata$rp110590.qp; xdata$rp110590_bk1.imh . ... xr> ximages xi> imcalc input file ('-' for STDIN) or imcalc commands: - # Interactive mode IMC) IMC) rp90_a.imh = xdata$rp110590.qp[bl=30,pi=7:240] - xdata$rp110590_bkl.imh # Select same size and channels as the background map # and subtract the background IMC) quit # To exit the interactive mode and imcalc . ...

... fi vig fi vig tan fi ; for fi ? fi vig ; (1) with fi vig = 2:97873882195 deg. ... The following effects of the LSF are parameterized: ffl all geometrical distortions of the surface of the XRT shells ffl scattering due to reflection of the XRT ffl all geometrical distortions of the surface of the RGA gratings ffl scattering due to reflection of the gratings 1 First, these items are convolved and are parameterized as a function of dispersion angle, resulting in an initial function of an LSF. ...

... We study an algebraic equation P (x, y ) = 0 over a field Fp , where p is a prime. ... p We study the upper bound of the number solutions of the polynomial equation, such that x g1 G, y g2 G. The estimate #{(x, y ) | ... This estimate was obtained by a different method in the paper [1]. ... 3] (With S. Makarychev) The number of solutions of polynomial equation over the field Fp and new bounds of additive energy // Proceedings of the Conference Diferential Equations and Related Topics, 2015, p. 24-26...

... 8, ``Celestial Mechanics'', 2002 FCN -- period dependence on dynamic characteristics of a lunar core A. Gusev 1 , N. Petrova 1 , N. Kawano 2 , and RISE group 2 1 Kazan State University, Kazan, Russia 2 National Astronomical Observatory, Mizusawa, Iwate, Japan Two modes in a polar oscillation are obtained when a free rotation of the two--layer Moon was studied: 1 PCW = 2\Omega A Am p fffi ё 1 74yr 1 P FCN = \ Gamma \Omega A 2Am ` C c \ ...

. Information for your local site should be placed here.

... Tpram - time of the PRAM instrument (aquisition computer) . ... Bx - DC magnetic field with a fixed amplitude calibration; X component . ... The color lines present FFT from the AC magnetic field (Waveform); Bwx, Bwy, Bwz - from the bottom. ...

... 2009: . ... New Wolf-Rayet Type Star. ... It was discovered that the peculiar velocity of the star is about 50km/s, and that it was discarded from a young star cluster. ... Based on the observational data from the 6-m telescope and from other sources, it was shown with high reliability that chemically peculiar stars with strong depressions in their continuum energy distributions possess the magnetic fields and rotation periods 2 and 3 times larger, respectively, than the stars with weak depressions....

... 30, 2006 . ... If you retrieve these files via a Web browser, please note that you need to use the browser's "Save As..." facility. ... Figures must be provided as Encapsulated PostScript files and should be incorporated in your contribution using the standard Latex2e "graphicx" package as demonstrated in the demo file author.tex. ... Please submit the LaTeX source file of your contribution, and PostScript/PDF files of any figures, via email (!!!) to Iris Bronnert ( ibronner@eso.org ). ...

... The target area that we are concerned with in this study has a few problems....in that there isn't an abundance of literature available for the individual to access in search of photographs of the target galaxies, and magnitude sequencing of stars around these galaxies. ... The Rev. Robert O. Evans of Coonabarabran, Australia. ... Reference photographs (no sequencing) of the target galaxies (with the exception of 27 galaxies) can be found in the Deep Space CCD Atlas: North, by John C. Vickers.( ...

... This example shows the Interference removal for the Baker Electron Density data (Qihou Zhou). ... The Arecibo ISR can measure velocities to an accuracy within 1 m/s for an integration time of 30 second in the D-region. ... The Arecibo ISR can measure the neutral winds and temperature in the E-region. ... We are working on to get the ion neutral collision frequency as well. ... The other parameters that we regularly measure include electron temperature, vector ion drift, light ion contents etc. ...

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on our photometric analysis of the poorly studied cataclysmic variable in Ophiuchus, 1RXS J174320.1-042953 (DDE 11). ... The long-term behavior of J1743-0429 shows that it is a probable magnetic cataclysmic variable (polar), with a large difference between its low and high states. The orbital period obtained from our observations is 0 0866, or 2 08, close to the lower boundary of the period gap of cataclysmic variables. ... Fig. ...