... The properties of the dust grains (e.g., temperature and mass) can be derived from fitting far-IR SEDs (т??100 ЮМm). Only with SPIRE on Herschel has it been possible to get high spatial resolution at 200 to 500 ЮМm that is beyond the peak (~160 ЮМm) of dust emission in most galaxies. Aims: We investigate the differences in the fitted dust temperatures and masses determined using only 200 ЮМm data is for deriving these dust properties. ...

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• Galactic FUV Extinction Determined Using FUSE
• STScI Preprint #1255
• LRPG DAILY PROCEDURE

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• THE HUBBLE LAW JAVA APPLET
• Historical Cosmologies
• Introduction to Sampling

... Keywords: Proper Motions, Schmidt Plates, Astrometry, Guide Star Catalog, Palomar Sky Survey . In this paper we describe a program of determining proper motions from digitized scans of 1950's-era Palomar Sky Survey (POSS) Schmidt Plates and 1980's-era Palomar Oschin Schmidt `Quick V' plates that were taken for the Hubble Space Telescope ( HST ) Guide Star Catalogue. ... Arrows indicate the magnitude and direction of the proper motion for the stars. ...

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• A Method for Minimizing Background Offset Errors When Creating Mosaics

... 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....

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• topic_en
• IRAS01005+7910
• HD965

... User Guide ] Task: gpnorm Purpose: Correct the polarisation leakage terms for an offset. Categories: calibration GpNorm is a MIRIAD task which corrects gains and polarisation leakage tables for XYphase and leakage offsets. ... GpNorm compares the leakage terms with nominally correct terms, and determines an leakage and XY phase offset to add which will minimise the difference between the two sets of leakages. ... No default. Key: cal The data-set containing the nominally correct leakage table. ...

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• Self-Calibration
• Determining Calibration Solutions
• PRECDATE

... The most precisely determined characteristic for accreting neutron stars (NS's) is their period. ... Period changes show fluctuations. ... Some applications of stochastic processes in astrophysics especially in accreting systems were discussed in Lipunov (1987),Hoshino Takeshima (1993) and Lipunov (1992).In Hoshino Takeshima (1993) the authors, using simple models of MHD turbulence, try to explain aperiodic changes in X-ray luminosity of X-ray pulsars. ... Here, -constant angular momentum. ...

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• No Title
• World Wide Web version
• E-P transitions for different orbits

Next: Reduction procedure Up: Extinction and transformation Previous: Strategy . Standard stars can be included in the extinction solution, if one is careful. The problem is that there are usually appreciable ``conformity errors'' due to mismatch between the instrumental and the standard passbands [ 16 ]. ... Thus, it is wrong to assume that the transformation between the instrumental system and the standard system is exact, even if there were no measurement error in either system [ 1 ]. ...

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• Upper Limits for Sources not Detected
• TESTTA/CCD
• Hierarchical Wiener filtering

Astronomy Picture of the Day . ... The different colors of this planetary nebula are determined by small differences in its composition. This bipolar nebula will continue to shine brightly for only a few thousand more years, after which its central star will fade and become a white dwarf star. ... Publications with keywords: bipolar - planetary nebula - butterfly nebula . Publications with words: bipolar - planetary nebula - butterfly nebula . ... NGC 3132: The Eight Burst Nebula . ...

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• Journal "Peremennye Zvezdy"
• Астронет > NGC 6302: The Butterfly Nebula
• Perihelion and Aphelion

The primary purpose of KM-7 is to measure the temperature of cold electrons Te in Plasmasphere. ... The spacecraft potential can be evaluated from these measurements. ... MLT . ... Fig.1 . KM-7 measurements in MRK mode during the whole orbit 124 , 27.IX.96. ... Preliminary results . In period considered SC passed the plasmasphere at low and middle latitudes near L < 4 at heights = 8000-10000 km. At L > 4-5 and heights > 8000-10000 km SC was in auroral zone. ...

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• STDA files
• The INTERBALL Auroral PROBE orbital elements collections
• Space Research Institute (IKI) Seminar

STANDART (ZONE) TIME is a medium solar time, determined for the 24 general geographical meridians, being 15* in longitude. The Earth surface is divided into 24 hour zones (with numbers from 0 to 23) where zone time coincides with the time of the prime meridian passing through these zones. ... The zone time of some zones has it’s own name, for example the zone time of the zero zone is called West – European (universal); the zone time of the second zone is called East-European. ...

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• antichnoste

The azimuth encoder rack gear is mounted on the inside of the azimuth ring girder. The azimuth encoder turns on this gear as the azimuth moves 0 to 720 degrees. ... The software assumes that this arc length along the encoder rack gear is correct (at a constant radius of 127/2 feet). The error in the radius of the rack gear becomes an azimuth error. To measure the error in the azimuth encoder rack gear, jon hagen built a proximity sensor. ... To compute the az encoder runout error: . ...

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• nearFarField

... Determining the nominal roll angle for stable intervals . ... We found the necessary information in a file 'rh*.ao', which has a binary extension table for each obi. ... Unlike the question of determining the nominal roll angle, we know of no a priori indication of this problem (although the guide star configuration may be the cause, or at least associated with this condition): it is necessary to examine the source position for each obi. ... The guide star record is at the end of the 'anc file'. ...

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• Stars with Less Secure Periods
• *imcnts* - Azimuthal profile of an extended source
• Determine a background subtracted radial profile

... They were determined as a result of orbit improving on the base of all kinds of optical observations available in the catalog of observations of the Minor Planet Center on March 16, 2014 (radar observations have not been used at this stage). ... As the MPC orbits do not all were improved simultaneously with EMP orbits, only 383866 sets of elements were used for data comparison (for selected sets of elements process of improvement had started with the use of the same observations). ...

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• Keywords_222
• Values of asteroid masses
• Keywords_17

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. ...

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• http://www.gao.spb.ru/english/personal/malkin/publ/zm03d.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/vavilov.pdf

The ESA/ESO Astronomy Exercise Series 2 . The Distance to Messier 100 as Determined by Cepheid Variable Stars . ... The small variations in distance to the individual Cepheid variable stars in the Cloud are negligible compared with the much larger distance to the SMC. ... In this way Cepheid variable stars can be used as one of the 'standard candles' in the Universe that act either as distance indicators themselves or can be used to calibrate (or set the zero point for) other distance indicators. ...

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• ASP: Determining the Earth-Sun Distance Using Mars
• ASP: Mercury Spring 2011

Physica C 1 PHYSICA C C ELSEVIER CONDUCTIVITY and Antiferromagnetism of CaCuO2 Thin Films Doped by Sr Gennady A. Ovsyannikova,b*, Viktor V. Demidovb, Yuli V. Kislinskib, Philippe V. Komissinskia,b, Dag Winklera a Chalmers ... revised date here; accepted date here Abstract The results of electrical and magnetic investigations of epitaxial CaxSr1-xCuO2 ( CSCO ) thin films grown by pulsed laser deposition are presented ... Temperature dependence EPR amplitude for two CSCO films with =0.15 ...

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• Project 8 - RFBR - Dynamical and non-equilibrium electron transport and

... Development of Ideas of Structure and Evolution of Stars. Integral Features of Stars, Which Determine Their Structure, Direction and Rate of Evolutuion. ... Connection between Potential and Thermal Energy of Star. ... Structure of a Main Sequence Star. Features of Massive Stars Evolution on the Main Sequence. Internal Structure of the Sun. ... White Dwarfs, Their Features. ... Evolution from the Main Sequence of Massive Stars. ... Evolution of Small Mass Stars till White Dwarfs Sequence. ...

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Our goal is to determine the orbit of Mizar A. We have reduced, calibrated, and imaged a single night of data which should enable us to determine the separation and position angle of Mizar on that night. The image provides a good guess as to these numbers, but we like to improve them by modeling. In the course of that, we also determine the magnitude differences between the component stars of Mizar. With the results from other night's data we will be able to determine the orbital elements. Continue

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• Marina Rejkuba's Web Site
• ASTROMETRYFIT
• NPOI Lab

This layer is defined with a <LAYER> tag. You see that the background image is applied to the rectangular region occupied by the layer. The height of the filled-in area is determined by the height value. ... The style definition sets the background-image property. The height of the filled-in area is determined by the actual content. ... The style definition also includes a value for border-width and border color. ... The style definition includes a value for layer-background-image. ...

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Next: DIRECT MASSES FOR BXCIR Up: EXTREME HELIUM STARS: PULSATION Previous: PULSATION PROPERTIES . As already indicated, V652Her is an important EHe star because its relatively short pulsation period and large amplitude pulsations allow its overall dimensions to be determined with high precision. ... Saio & Nomoto (1998) made the first successful models for the merger of two carbon-oxygen white dwarfs, and prompted Saio & Jeffery (2000) to attempt models for the merger of two helium white dwarfs. ...

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• A Statistical Study of the Relationship between the Solar Cycle Length and
• Armagh Observatory
• Low-Mass Star Formation