... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

... ОБ ОТДЕЛЕ . ... Cеминар теоретического отдела АКЦ ФИАН . ... Новости со школы 'Струны и дуальность' . ... Председатель д.ф.-м.н. В.Н.Лукаш. Секретарь к.ф.-м.н. Е.В.Михеева ( helen@lukash.asc.rssi.ru ), . ... Пропуска заказывать у секретаря АКЦ Страут Людмилы Георгиевны по телефону 333-25-12 до 12 часов предыдущего дня, для прохода в ИКИ при себе иметь паспорт. Новости . ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... The hydrogen line is the most pronounced absorption feature in spectra of B-type stars. Two effects play the dominant role in observed behavior of : the Stark broadening of the line absorption coefficient and interstellar absorption. ... Keywords: B-type stars, H I line, Stark effect, interstellar absorption . ... Thus having a good description of the Stark effect we investigated early B-type stars, where interstellar absorption may play an important role. ... 4 (IUE observations) and Fig. ...

... ТЕОРЕТИЧЕСКИЙ ОТДЕЛ . Заведующий отделом . ... Ахметьев П. М. Белый В. В. Волокитин А. С. Дворников М. С. Кутвицкий В. А. Леинсон Л. Б. Маслов Е. М. Молотков И. А. Рашба Т. И. Тарбеева С. М. ТЕОРЕТИЧЕСКИЙ ОТДЕЛ . Физика нейтрино и нейтринная томография внутренних областей Солнца . ... Физика нейтрино в компактных астрофизических объектах . Нелинейные процессы в темной материи . ... Нелинейные волновые процессы и нелинейные структуры . ...

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

. Next: References Up: RGS_LINESPREADFUNC Previous: Ground calibration Contents . The CCF model LSF is nevertheless subject to verification in-flight by comparison of 1st and 2nd order data ideally of narrow-lined sources with spectral models in XSPEC for example, calculated using RGS response matrices calculated by the SAS. Michael Smith 2011-09-20

energy levels (n=2): Edlen, B, 1983, Phys. Scripta, 28, 483 %energy levels (n=3): Martin,W.C., Sugar,J., Musgrove,A., Dalton,G.R., 1995, NIST Database Version 1.0. %comment: energy of level 55 estimated by comparison with Sampson's values %theoretical energy levels: Sampson and Zhang, 1995, unpublished calculations %produced as part of the Arcetri/Cambridge/NRL atomic data base collaboration % % K.P.Dere and E.Landi 1999 . ...

PERFORMANCE COMPARISION OF KODAK DCS460 DIGITAL CAMERA AND PIXELVISION BACK-ILLUMINATED CCD . ... ABSTRACT : A Kodak DCS460 digital camera (with 1300 x 1000, 9-micron square pixels) and a PixelVision, back-illuminated digital CCD camera (with 1024 x 1024 elements, 12-micron square pixels) were tested at calibrated light levels ranging from 10 -2 footcandles to 10 -5 footcandles. The PixelVision back-illuminated CCD was shown to be 10,000 more sensitive than the Kodak DCS460 CCD camera. ...

... ATNF Home . ... About ATNF overview . ... Parkes radio telescope . ... The Monash Spectrograph Simulation Program . ... As mentioned previously, the results from the MSSP were to be compared with actual results from the completed Monash spectrograph. ... We compared the calculated theoretical count-rate for a star of a paticular visual magnitude using the RGO spectrograph, assuming that it is situated on the Monash telescope, with the count-rate predicted by the MSSP for the Monash spectrograph. ...

Collection of the orbital elements | ... The errors of the spacecraft motion extrapolation outside the measuring time interval were estimated by using the comparison of SC positions calclulated by the forward integration ( extrapolation method) and backward integration ( interpolation methods). ... The character of these time shift of the ascending nodes ( D Tn) corresponds to the orbiting period errors, which arise during SC motion extrapolation outside the measuring intervals. ... INTERBALL mission ...

Calibration of ALFA data in LiveData R. Minchin Abstract The calibration factors to be entered into LiveData have been calculated, for the parameters used for the AGES and ZOA E-ALFA pro jects and a method is described for calculating these more generally. ... The calibration factors 1 2 Testing the calibration http://www.naic.edu/~ rminchin/alfacal.shtml Three AGES cubes have so far been constructed using this calibration: the completed NGC 1156 and NGC 7332 cubes and the incomplete Abell 1367 cube. ...

... Bojan Nikolic web pages home . Next: Fitting of models of radio spectra --.. ... I describe an approach to fitting and comparison of radio spectra based . on Bayesian analysis and realised using a new implementation of the . ... used maximum-likelihood fitting of radio spectra by allowing objective . ... implementation details of the computer code. ... overall approach described here may also be useful for analysis of other . ... Copyright 2012, Bojan Nikolic feedback welcome ...

Hide Zen home . ... Index . ... Do we really need them for database indexing ? ... We need simple numbering scheme, so that for any given point we could easily calculate the number of "pixel", this is what HealPix provides and lacks HTM. ... During Rtree queries the number of index blocks read is several times greater than during Q3C queries. ... But in Q3C scheme, as we showed before, the circle is segmented, so we extract from the database only a few percents more data than occur in the circle. ...

... The x-ray spectral analysis consists of a comparison between the observed pulse height spectrum and a pulse height spectrum calculated using a given spectral model. ... To obtain the spectral parameters for an x-ray source, several steps need to be followed. For each source: . ... obtain the best fit parameters for a spectral model - repeated for each model of interest . obtain a 1-D or 2-D grid of values around the best fit values - this can be done for as many models as desired . ...

... Spectral density of atmospheric pressure term around the FCN frequency Amplitude modulation of signal a(t ) A(t ) cos(0t 0 ) A(t ) A0 A cos(t ) A0 [1 m cos(t )] MA0 a(t ) A0 cos(0t 0 ) cos[(0 )t (0 )] 2 MA0 cos[(0 )t (0 )] 2 Annual variation of amplitude of S1 tide Semiannual variation K1; P1 1; 1 S1 (t ) A cos 2 f S1t B sin 2 f S1t Amplitude modulation of complex signal P 430 (410; 480) f 1.002324 (1.002439; 1.002083) f modulation (0.000115 0.000241) Pmodulation (8700 6100) 18.6 years? ...

Next: Determination of atmospheric parameters Up: Optical spectrum of IRAS04296 Previous: Radial velocity of the . From comparison of observed and synthetic spectra of IRAS04296 we revealed some strong absorptional features whose positions coincide with known diffuse interstellar bands (DIBs) (Jenniskens et al., ... In Fig. 5 we illustrate the presence of DIB's by showing a spectral region of IRAS04296 . ...

We investigate models for main-sequence and horizontal-branch (HB) stars constructed using the Carson opacities and make comparisons with models based on the Cox-Stewart opacities. ... The drop in the hydrogen-shell luminosity due to the helium-core expansion during HB evolution is greater than that obtained with the Cox-Stewart opacities. ... Studies of main-sequence (MS) stars lead to agreement with Stothers' (1974a,b, 1976) results for homogeneous models constructed with Carson opacities. ...

Астрофизический семинар АКЦ ФИАН . ... Секретарь к.ф.-м.н. В.С.Бычкова . bychkova@asc.rssi.ru ), контактный телефон 333-25-12 . Заседания проводятся по понедельникам в 15 часов, к. 718 в здании ИКИ . ... Пропуска заказывать по телефону 333-25-12 до 12 часов пятницы, . для прохода в ИКИ при себе иметь паспорт. ... back to ASC main page . ... helen@lukash.asc.rssi.ru ), контактный телефон 333-33-66 . Заседания проводятся в 15 часов объявленного дня, к. 733 в здании ИКИ . ...

... The package AMPLE (Adaptable Minor Planet Ephemerides) is dedicated to solving a number of problems concerning minor planets with the aid of IBM-type personal computer. ... Obtaining selection of orbital elements and/ or photometric parameters of minor planets in conformity with imposed restrictions. ... The orbital elements of all minor planets used in AMPLE for 2015 have been determined in IAA on the ground of available observations in the catalogue of observations of the Minor Planet Center. ...