The summary plot shows the monthly time distribution of all predicted magnetic conjugations between four spacecraft considered. ... To show the time of conjugation, in frame of the corresponding day for each SC the corresponding colour and line are used: . for the first SC the red color and the first line are used, . ... On the plot the SC names are shown by the corresponding colours. The summary plot permit to find the simultaneous magnetic conjugations of 3 and even 4 satellites. ...

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• The FSP3 criteria and plot description
• The plot of the magnetic conjugation's time distribution
• Situation investigation for using during IACG/ISTP Campaign 2 scheduling

Cherechukin A.A., Koledov V.V., Shavrov V.G., Tulaikova A.A., Vasil'ev A.N. Magnetic and structural phase transitions in Ni2+УMn1-УGa (0<У<1) alloys are investigated experimentally. The martensite domains formation under the action of external magnetic field on the surface of polycrystalline Ni2,19Mn0,81Ga specimen was investigated by optical method. ... It is found that the martensite phase formation temperature is enhanced by the order of 0,3 K in magnetic field of 1 kOe. ...

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... Evolution of the magnetic field (solid lines) , temperature (colour) , and velocity (arrows) at four times for case A1 (a), A2 (b), B1 (c), and B2 (d). The characteristic parameters of magnetic field strength and electron number density are given above each case plot. ... Aims We aim at investigating the formation of jet-like features in the lower solar atmosphere, e.g. chromosphere and transition region, as a result of magnetic reconnection. ...

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• Coronal Bright Points: Another Oscillating Environment

Dynamical chaos in the problem of magnetic jet collimation O. Yu. ... In the paper of Bisnovatyi-Kogan (2007) magnetic collimation resulting from torsional oscillations of a cylinder with elongated magnetic field and periodically distributed initial rotation around the cylinder axis was considered. ... Space and time periods of oscillations depend on the conditions of jet formation: the length-scale, the amplitude of the rotational velocity, and the strength of the magnetic field. ...

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• http://hea.iki.rssi.ru/integral06/papers/G41_Schoenherr01-07Feb07_16:54:04.pdf

NGC 1569: Heavy Elements from a Small Galaxy . ... CXC , NASA Explanation: For astronomers, elements other than hydrogen and helium are sometimes considered to be simply "heavy elements". ... Still, heavy elements can profoundly influence galaxy and star formation ... not to mention the formation of planets and people. ... The furious cosmic activity has heated the expanding gas clouds to temperatures of millions of degrees while enriching them with newly synthesized heavy elements. ...

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• NGC 1569: Heavy Elements from a Small Galaxy
• XWare > APOD

Text of report The subject if our report is the influence of the structure and physics of the uppermost superadaibatic layers on the oscillational spectrum of p-modes. ... In our report we will try to use a most simple representation of the spectrum, plotting the differences between theoretical (that is models') and observational frequencies against a frequency. ... It allow us to focused on the effects of the uppermost layers and ignore possible sophistications from effect of more deeper layers. ...

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• http://crydee.sai.msu.ru/~mir/fulltext_mir.pdf
• ApSA courses

... According to the current estimates, a few percent of Main Sequence B5-F5 stars reveal strong surface magnetic fields reaching the values of tens of kilogauss, which is an order of magnitude greater than the maximal magnetic field in sunspots. ... An important direction in the study of magnetic stars is the study of binary and multiple systems with magnetic components using the techniques of spectroscopy and high angular resolution interferometry. ...

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• Galaxy sector, archive 2012
• Metagalaxy sector, archive 2010
• Galaxy sector, archive 2008

... V.K. Dubrovich . ... It is shown that some primordial molecules could produce low-frequency photons (which correspond to the rotational lines) by decaying high-frequency rovibration photons from the CMBR. ... They are the so-called SSF - Spectral Spatial Fluctuations ( Dubrovich, 1994 ). ... For obtaining the greatest interaction between molecules and photons, two values are important - the cross-section for scattering and the concentration (or relative abundance) of this molecule. ...

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• Emission molecular bands
• Результаты научных работ 25

... The distributions of orbits eccenttricities and of angular momenta for the halo stars and the old disk population are considered. The distributions have gaps separating the halo from the disk and dividing the halo population into three groups. ... Рассмотрены распределения звезд гало и старого населения диска по величине эксцентриситета орбит и угового момента. Распределения имеют провалы, отделяющие гало от диска и делящие населения гало на три группы. ...

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Blackholes2 Forum Message . Forums: . Atm ћ Astrophotography ћ Blackholes ћ Blackholes2 ћ CCD ћ Celestron ћ Domes ћ Education . ... Post . ... Could This Be Considered The .. ... Post Message | ... www.astronomy.net . About Astronomy Net | ... Unless otherwise specified, web site content Copyright 1994-2016 John Huggins All Rights Reserved . Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

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• I Think What You're Saying Is Not A Deeply-considered Position - an Astronomy
• Ragamullen@yahoo.com - an Astronomy Net Blackholes2 Forum Message

... stars . ... Could gas giants be considered stars that failed to ignite? ... The distinction between gas giant planets and brown dwarfs ("failed stars") is a vague one. ... It depends on what gas giant youт??re looking at and how you distinguish a т??planetт?? from a т??failed star.т?? A gas giant found in orbit around a star might be considered a planet like Jupiter around the Sun. An isolated gas giant is probably a failed star. ... Get instant access to subscriber content on Astronomy.com! ...

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Next: Scattering properties Up: Polarization properties (transmitted radiation) Previous: Linear polarization: wavelength dependence . Traditionally, the main problem considered in connection with circular interstellar polarization is the meaning of the wavelength where changes the sign . ... This is also demonstrated by Fig. 19 (lower panel) which shows the wavelength dependence of the factors of linear and circular polarization for particles of magnetite as was done by Shapiro ([ 1975 ]). ...

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• intro3e
• Database of Optical Constants -- Level: welcome
• Polarization properties (transmitted radiation)

... In Figures 2-2, 2-3, 2-4 spot diagrams corresponding to the minimum dispersion configuration at zenith, maximum dispersion at 60° and ADC compensation at 60° are shown. ... Date:04.06.98 Page 2 of 6 Figure.2-1 Camera and ADC with curved surfaces in the maximum dispersion configuration Figure.2-2 Spot corresponding to the configuration of minimum dispersion at zenith 2 Document : VST_040698_optic.doc Release :1 First rel.date: 04.06.98 Last rel. ... Date:04.06.98 Page 5 of 6 Figure. ...

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• Space spaghetti in magnetic sauce
• Deadlines - IGM@50: Is the Intergalactic Medium driving Star Formation? - June
• Dust grains from the heart of supernovae

Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System Characteristics Formation Exosolar Planets Class 3 Stars The S un Stellar Evolution of Low and High Mass Stars Deaths of Stars Exotic Stars Class 4 Galaxies Galaxy Classification Formation of Galaxies Galactic ... Low mass stars live and die differently than high mass stars. ...

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... Introduction: E-, M- and S-type asteroids are widely considered as remnants of differentiated parent bodies; specifically, Ms might have been their cores [e. g., 1, 2]. The conviction is based on the visible-range albedo (medium to high) and overall spectral curves (slightly reddish to red) of the small planets corresponding to these of metal iron and igneous silicate assemblages. ... It seems the spectral features superimpose to the spectral characteristics of metal iron and igneous silicates. ...

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• http://selena.sai.msu.ru/Symposium/RadioMoonE.doc
• http://selena.sai.msu.ru/Symposium/RadioMoonE.pdf
• http://selena.sai.msu.ru/Kozl/Publications/Houston2005(1).pdf

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. ...

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• Application of the Minimum Determination Algorithm to the Study of the Fine

... To determine a lower limit to the sensitivity of current observations to measurements of NS surface temperatures, we have used data from the Einstein Slew Survey (Elvis et al. 1990) to establish temperature limits for 275 pulsars which received nonzero exposure during the survey. ... Filled squares correspond to pulsars actually detected in the survey data; the smaller symbols correspond to upper limits to the count rates. ... Click here for plot of x-ray data vs. cooling curves. ...

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• Very Low Mass PMS Objects
• Use of Cookies Considered Safe
• The AstroStat Slog star formation

... Intuitive model Step 1 Step 2 Step 3 Predictions This simple theory leads to a number of, potentially, observable predictions (1) The ejection speed of the flow increases as one approaches the star (2) Stellar rotation period may be a fundamental period of the flow (3) The flow starts at Rt and ends at Ro when the transfield current runs out Current balance equation Predictions Mass ejection is proportional to mass accretion ... Inner disk dust ~ 90% crystalline silicate. ...

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• ATNF Divisional Awards
• Australia Telescope National Facility
• ATNF Colloquium

MUON METHOD FOR A MATTER STUDYING Yu. ... З МТЪУflВВ , ВПfl ПУММњИ ПВЪУ Оfl ЩЛБЛНЛ Л iЛПЛЛ НУМВМТЛУ,ММњi Л ,,БУУћ БМњi ЩБ ЛПВВЪ ЪНУВ КВ БМ~ВМЛВ, НН ПВЪУ flВ МУ,,У П,,МЛЪМУ,,У ВБУММТ ЛОЛ ПfiТТћЫУ,ТНfl ,,ПП-ТФВНЪ УТНУФЛfl. ы. е. ЕЦгймлйЗ, З. и. леагЙД еУТНУ,ТНЛИ ЩЛБЛНУ-ЪВiМЛ~ВТНЛИ ЛМТЪЛЪЫЪ, СУО,,УФ ЫМњИ еУТНУ,ТНУИ УћО. ЗЗЦСЦзаЦ 76 ї ЕВОУЫТУ, ы.е., лПЛО,, З.и., 1999 : ( ), , , чSR-, , . чSR . ... ЕЦгймлйЗ ы.е., леагЙД З.и. унй нДдйЦ еыйззхв еЦнйС аллгЦСйЗДзаь ЗЦфЦлнЗД 77 M mr. : . ... 3) : cos | ...

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... Space Res., 12, 265, 1992 planetary magnetic dipole: Mizutani, H., et al., ... Astrobiology, 7, 167, 2007 CME induced H+ ion pick-up loss at 0.05 AU for ` Hot Jupiters ' HD209458 b Mass loss ~1011 g/s even for weak CMEs Mmax strong magn. protection in reality Exoplanet magnetospheres - importance of magnetodisk Relatively large amount of observed Hot Jupiters (27%): survival of close-in giants indicates their efficient protection against of extreme plasma and radiation conditions ...

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• http://solarwind.cosmos.ru/txt/2011/presentations/Sun/Kuznetsov/JASR2006-S-06-01000.pdf