... ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Astrophysics graduate student programs . ... Australian Square Kilometre Array Pathfinder . Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Visiting Parkes radio telescope . Visiting Australia Telescope Compact Array . ... Parkes radio telescope webcam . ...

... X-Ray Structural Analysis . ... The course introduces the basic principles of diffraction analysis of crystal atomic structure and the basic concepts of state-of-the-art atomic crystallography. ... X-ray crystal diffraction. тАЬGeometricalтАЭ theory of diffraction by three-dimensional scattering center grating. ... Systematic X-ray reflection extinction related to Bravais lattice type, screw axis, glide-reflection planes. €аFourier synthesis as a method of crystal atomic structure analysis. ...

... CALIBRATE/LINE Calculate coefficients for wavelength calibration . CENTER/.. Compute center of line . CONVERT/TABLE Make image from table values . EXTINCTION/SPECTRUM Correct 1-D image for extinction . IDENTIFY/GCURSOR Identify table entries from graphic display . IDENTIFY/LINE Equate X positions to wavelengths . INTEGRATE/GCURSOR Integrate line interactively . MODIFY/GCURSOR Change data in line interactively . ... SEARCH/LINE Search calibration lines . ...

Tail Probe is one of the satellites of the INTERBALL program. ... Collection of the orbital elements | ... Flight situation analysis during operations scheduling . ... Two stages of the orbital situation analysis are presented: . ... The satellites motion calculation during the flight situation analysis is based on the orbital elements, determined by the Ballistic center at KIAM RAN. The modified (by backward integration) orbital elements are usedduring the aposteriory situation analysis. ...

SPECTRUM ANALYZER OF MAGNETIC PHENOMENA SAMW . Spectrum analyzer allows onboard computation of electromagnetic waves spectra registered (observed) in the ionosphere and magnetosphere in the ELF/VLF frequency band. ... It consists of magnetic antenna, preamplifier, 16 bit sigma delta AD converter, DSP processor and telemetry interface. ... The channels of lower frequencies are averaged and transmitted with lower repetition rate so the telemetry volume is reduced. ... Dynamic range: 90 dB . ...

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... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Last modified . ... 2011-06-09 11:56 . ... 860K . ... 835K . ... Last Revised: 2013 April 25th . ...

... PUL VLBI Analysis Center . ... Pulkovo EOP and Reference Systems Analysis Center (PERSAC) is located at the Pulkovo Observatory . ... Processing of VLBI , GPS, and optical observations aimed at analysis of the Earth rotation, station displacement, and celestial reference system. ... Celestial Pole Offset (CPO) and Free Core Nutation (FCN) . Four daily updated CPO and FCN series (models) are provided. ... File fcn1.dat contains the ZM1 FCN model with variable amplitude and phase. ...

... Previous: Determination of Variable Time Delay in Uneven Data Sets . ... It is shown that the likeness of the periodogram and the LS-spectrum (both estimators of the power spectrum are widely used in the spectral analysis of time series), depends on the properties of the spectral window corresponding to the distribution of time points. ... Present day theory and practice of the spectral analysis of unequally spaced time series are based on two approaches. ...

Next: Evolution of Magnetic Rotators Up: ``Ecology'' of Magnetic Rotators Previous: The equilibrium period . The evolution of NS in binaries must be studied in conjunction with the evolution of normal stars. ... Figure: Tracks of NS on the period ( p ) - gravimagnetic parameter ( Y ) diagram: track of a single NS (vertical line) and of a NS in a binary system (looped line). ... Another version of the evolutionary track of a NS formed in the process of mass exchange within a binary system is: . ...

... temporal activity in stellar atmospheres and signal processing of spectral data. ... 1) 1996: Found X-ray/UV/optical link of initial outburst event in a Be star. 2) 1996: Resolved radiative transfer problem concerning equal emissions of . singlet triplet lines of HeI lines in Be star spectra. ... 4) Late 1970's: Discovery of a new class of variables (nonradial pulsating B stars). 5) Mid 1970's: Application of Fourier techniques for optimized signal recovery . of spectral line profiles. ...

Please enter the lightcurve file name and period search parameters: . Lightcurve file: . ... Apply the Heliocentric correction and convert all dates to Terrestrial Time (TT)? ... Also, the Heliocentric correction cannot be applied to such lightcurves. ... This period search service is also available at the mirror sites: Mirror 1 , Mirror 2 , Mirror 3 , Mirror 4 . You may download the latest source code distribution and install the period search service at your own web server. ...

... Because of the low conductivity, the magnetic coupling is weak and depends critically on density, temperature, ionisation rate and charged species. ... Implications When the Hall regime dominates near the midplane and ambipolar diffusion is dominant closer to the surface, a thicker layer of the disc is unstable to MRI perturbations and modes grow faster than under the ambipolar diffusion approximation. ... Right panel: For weak coupling, Hall limit perturbations grow until vA/cs ~ 2.9. ...

... The task makes use of a source-list produced by running omdetect on the same image. ... Parameter Mand Type Default Constraints set yes string OM image le with grism spectra aligned with respect to the columns of the image ( output from omg- prep). xmmsas 20041122 1834-6.1.0 XMM-Newton Science Analysis System Page: 2 sourcelistset yes string Source list ( output from omdetect) outset yes string Output spectra le region le no string Name of the ASCII (input) ...

Magnetic Stars, 2011, pp. ... We discuss our most recent determination of the rotational period from longitudinal magnetic field measurements and H variability -- the latter obtained from over a decade's worth of professional and amateur spectroscopic observations. ... We concluded that the dipolar field of HD 57682 is characterized by a polar strength of 1.7 kG, and a magnetic axis aligned within 10 to 50 of the rotation axis, depending on the inclination of the rotation axis to our line of sight. ...

Magnetic Fields around Radio Galaxies Robert Laing (ESO) Laing et al. ... 2008) Negligible depolarization and 2 rotation Almost all Faraday effects must be due to foreground material How to fit depolarization caused by foreground Faraday rotation Complex polarization Rotation measure Integrate over a beam Observed RM for 0 2 rotation and depolarization Faraday rotation and depolarization 5.5 arcsec FWHM Faraday effects at high resolution FWHM = 1.5 ...

... Microlocal Analysis is a theory of Pseudo-Differential Operators and Fourier Integral Operators (PDOs and FIOs). ... Microlocal analysis comes in few flavors. ... We will consider semi-classical PDOs and FIOs: one can always get from there to standard PDOs and FIOs but semi-classical theory has more applications. Less formal description of (semi-classical) microlocal analysis is ``a semi-classical limit of quantum mechanics'' or ``high-frequency limit of electrodynamics'' (etc). ...

CONTENTS : INTRODUCTION INSTRUMENTATION FOR MAGNETIC FIELD MEASUREMENTS Instrumentation for measurement of stellar magnetic fields with the 6-m telescope: Yu. ... 32 The bank of observational data for chemically peculiar stars: V. S. Lebedev .36 RESULTS ON MAGNETIC FIELD MEASUREMENTS A surface magnetic field study of Ap star 78 Virginis: T. A. Ryabchikova, E. S. Davydova, D. Z. Kolev Modern state of magnetic field investigation in M. Yu. ... Magnetic fields of superqiants: E. Gerth .. ...

. First page Back Continue Last page Summary Graphics . First cut, cross calibrate to Leiden-Dwingeloo (0.5 ) . This tends to smooth out total column changes on small scales, but preserves velocity features .

... 2009) 0 Fig.1 · Max-Planck-Institute for Radioastronomy, Bonn , VLBI ESO, COMPONENTS PARAMETERS FROM INTERFEROMETRY · Following S.Kraus et al. ... Using i=105o , we obtain v sini = 32 km/s. BEST MODEL FIT 1OriC 1 · Mass, M · Luminosity, log L · Radius, R · Teff, K · log g · Equatorial rotation velocity, km/s · Magnetic field , G · The time of life, yrs 35.8 5.20 10.0 37000 4.01 5.4 500-1500 150 000 1OriC 2 10.0 4.69 8.2 30000 3.60 96.2 moves to MS 1 OriC ...