... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

Еще в разделе: (Показать все результаты (>1043) - jet.sao.ru/ )

Next: A Gravitational Wave Map Previous: Critical Frequencies and Gravitational . In this section we consider the GWB spectrum as such, that is, we study how dimensionless strain metric amplitude h is dependent on frequency. For a sample of N independent binaries emitting GW at a given frequency the net result is . ... are, respectively, effective distance to the sample and effective mass of the binaries (in solar units) producing the GW radiation at the frequency . ...

Еще в разделе: (Показать все результаты (>537) - xray.sai.msu.ru/ )

• Initial Distributions of Binary Parameters
• Effect of sources evolution on
• Dependence on the Scenario Parameters and Initial Distributions

We present a database of UV-to-FIR data of 83 nearby starburst galaxies. ... The NIR data are from new observations obtained at the NASA/IRTF and the Mount Laguna Observatory, combined with the published results from observations at the Kitt Peak National Observatory. ... In conjunction with IRAS and ISO FIR flux densities, all these data form a set of observed spectral energy distributions (SEDs) of the nuclear regions of nearby starburst galaxies. ...

Еще в разделе: (Показать все результаты (>19083) - www.stsci.edu/ )

• Limitations on the Calibration Accuracy for COS/FUV Observations of Extended
• Three-Dimensional Dust Radiative Transfer*
• Correcting ETC Calculations of CCD Spectral Observations for CTE Effects

ESTIMATIONS OF EFFECTIVE HEIGHT, SIZE AND BRIGHTNESS TEMPERATURE OF SOLAR CYCLOTRON SOURCES A.N. Korzhavin, T.I. Kaltman Sp ecial Astrophysical Observatory of RAS, Saint-Petersburg, Russia arles@mail.ru The mo deling of microwave emission from a sp ot-asso ciated cyclotron source was done to refine the metho d of estimations of effective brightness temp erature, size and height ab ove photosphere in the pro cessing of RATAN-600 observations. ...

Еще в разделе: (Показать все результаты (>1979) - www.sao.ru/ )

• http://www.sao.ru/cats/~satr/RFSymp/abs/17_Korzhavin.ps
• Corrections to the probability distribution
• THE 4.85 GHZ NORTHERN SKY CATALOG

. This Directory contains Model of distribution of density, temperature and effective collision freguency of electrons. Yu.K.Chasovitin. 1998. This Directory contains The program RIM98 for calculating the parameters of the ionosphere to use the "Reference Ionospheric Model-98" (RIM-98).Yu.K.Chasovitin. 1998.

Еще в разделе: (Показать все результаты (>86) - www.wdcb.ru/ )

• "STP Data" STP Data
• Catalogue 5 of WDC-B

... We present a computer program for modelling energy flux distribution and light curves of eclipsing binaries from far ultraviolet to infrared regions. The Roche model is assumed. Proximity effects of components (reflection of radiation and surface gravity darkening) are taken into account. ... Figure 1: The surface temperature distribution for Algol A-B system before (upper plot) and after (lower plot) correction for temperature due to the irradiation effect. ...

Еще в разделе: (Показать все результаты (>1730) - www.adass.org/ )

• Distributed Software for Observations in the Near Infrared
• Modelling Spectro-photometric Characteristics of Nonradially Pulsating Stars
• A Test for Weak Cosmic Ray Events on CCD Exposures

Next: Pulsations Up: PHYSICAL CHARACTERISTICS Previous: PHYSICAL CHARACTERISTICS . The fundamental properties of RCBs may be deduced from their spectra at maximum light. ... The properties of a stellar atmosphere may be measured from both the large-scale features - the broad-band flux distribution - and the detailed spectrum of absorption lines. ... They show that, in general, hydrogen makes up less than one part per thousand down to less than one part per million of the stellar atmosphere. ...

Еще в разделе: (Показать все результаты (>2413) - star.arm.ac.uk/ )

• Armagh Observatory
• STELLAR PROPERTIES
• Stellar Atmospheres Software

... Marcus G. F. Kirsch XMM-Newton EPIC Page 2 CAL campaign 2007 The EPIC consortium together with the XMM-SOC will start a major (cross) calibration campaign in order to try to resolve pending calibration issues and to bring the EPIC calibration to the next higher level of quality. set of objectives local MOS and pn cal meetings be-weekly telecons Marcus G. F. Kirsch XMM-Newton EPIC Page 3 objectives · ... Marcus G. F. Kirsch XMM-Newton EPIC Page 9 ...

Еще в разделе: (Показать все результаты (>5817) - xmm.vilspa.esa.es/ )

• http://xmm.vilspa.esa.es/calibration/documentation/epic_cal_meetings/201203/stuhlinger-cal-2012-2.pdf
• http://xmm.vilspa.esa.es/docs/documents/CAL-TN-0159.pdf
• http://xmm.vilspa.esa.es/docs/documents/CAL-SRN-0135-1-0.ps.gz

... The main field of my investigations is stellar spectrophotometry. As a result of scientific activity of our group spectrophotometric catalog was created including energy distribution data on 900 stars in the range 3200-7600AA and 250 stars in the range 6000-10800AA (Voloshina et al., Spectrophotometry of Bright Stars, ed. I.N.Glushneva, 1982, Moscow, Nauka, in Russian). ...

Еще в разделе: (Показать все результаты (>18) - uranus.sai.msu.ru/ )

. Next: Diameters Up: Stellar parameters from calibrations Previous: Gravities Contents . Temperatures of stars are derived from their spectral type and luminosity class. Calibrations are stored in files spec_par.V, spec_par.IV, spec_par.III, spec_par.II, spec_par.I in oyster/starbase . teff_stars Compute effective temperature for all stars in startable. teff_star ( spectrum _char ) Function. Return effective temperature for star with specified spectrum. Christian Hummel 2015-04-28

Еще в разделе: (Показать все результаты (>21142) - www.eso.org/ )

• FORS1: Sky Flats and Rotator Effect
• FORS2: Sky Flats and Rotator Effect
• The Effect of Continuum Variability on Spectral Indices

An investigation of the spectral energy distribution (SED) of the compact steep-spectrum (CSS) source and possible radio-loud narrow-line Seyfert 1 galaxy (NLS1), PKS 2004-447, is presented. ... Analysis of a non-contemporaneous, low-resolution optical spectrum suggests that the narrow-line region (NLR) is much more reddened than the X-ray emitting region suggesting that the gas-to-dust ratio in PKS 2004-447 may be very different than in our own Galaxy. ...

Еще в разделе: (Показать все результаты (>17933) - www.atnf.csiro.au/ )

• The derived luminosity and spatial distributions
• Distribution of Schedule Files
• The IR Spectral Energy Distribution

... 2014: . Suppression of cooling by strong magnetic fields in white dwarf stars . ... 69, 439, 2014. Evidence of supercritical accretion in SS433 . ... We discovered a flat portion (white noise) in the power spectrum of SS433 due to an abrupt increase of the disk thickness in the supercritical region. ... Both the hard X-ray radiation and the visual light are seen reflected from the walls of the funnel that forms in the wind of the supercritical disk of SS433. ... Archive . ...

Еще в разделе: (Показать все результаты (>303) - mavr.sao.ru/ )

• Solar system sector, archive 2006
• Galaxy sector, archive 1997
• Physics of Magnetic Stars 2007

. Spectral Energy Distribution of the microquasar LS 5039. This is a composite: observations were not taken simultaneously. From Paredes, Bosch-Ramon, Romero, A , 451, 259 (2006).

Еще в разделе: (Показать все результаты (>3838) - hea-www.harvard.edu/ )

• The AstroStat Slog Blog Archive [ArXiv] Bimodal Color Distribution in GCS,
• Why Spectral Energy Distributions?
• The AstroStat Slog Blog Archive Redistribution

... It is reasonable to expect that UV part of the irradiating spectrum is most influenced by the grain evolution (growth and sedimentation ) which marks the very initial stage of planet formation. 2 log J [erg s­1 cm­2] 1 0 -1 -2 -3 1000 BB 40 0 0 (A5 ) BB 20 0 00 (A5) Drai ne (A5 ) BP Ta u (A5) BB 40 0 0 (GS) BB 20 0 00 (GS) Drai ne (GS) BP Ta u (GS) Disk Model Density distribution is based on a 1+1D disk ... Green lines are used for a model with dust growth and sedimentation. ...

Еще в разделе: (Показать все результаты (>36) - www.inasan.rssi.ru/ )

Еще в разделе: (Показать все результаты (>397) - zebu.uoregon.edu/ )

• http://zebu.uoregon.edu/tandf/toc.html
• http://zebu.uoregon.edu/messier/m2.txt
• Evidence for Dark Matter

Subject, Object and Problems of Astrophysics. Practical and Theoretical Astrophysics. ... Visual Telescope; Problems Which Are Solved with the Its Help. ... Resolution of Telescopes. ... Effectiveness of Telescope in Respect of Resolution. ... Optical Power of Telescopes for Star-like and Extensive Objects. Boundary Magnitude. Reasons of Light Dissipation in Telescopes. ... Spectral Instruments in Astrophysics. ... Basic Photometrical Ideas, Magnitudes and Their Measurement. ...

Еще в разделе: (Показать все результаты (>125) - space.univ.kiev.ua/ )

• Theoretical Astrophysics
• Extragalactic Astronomy
• Stellar Astronomy

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

Еще в разделе: (Показать все результаты (>259) - www.astro.spbu.ru/ )

• Linear polarization: wavelength dependence
• Database of Optical Properties -- Level: subpage
• Fractal Matter Distribution

Twilight observations with MASS/DIMM B. Safonov Sternberg Astronomical Institute Moscow State University Comprehensive Characterization of Astronomical Sites, 2010 B. Safonov (Moscow State University) Twilight observations with MASS/DIMM SITE 2010 1 / 17 Why observe in twilight with MASS/DIMM? ... ASM includes 3 devices sensitive to background: guider, DIMM and MASS. B. Safonov (Moscow State University) Twilight observations with MASS/DIMM SITE 2010 2 / 17 Background in guider. ...

Еще в разделе: (Показать все результаты (>25) - site2010.sai.msu.ru/ )

To main of Laboratory . The research work and design of optical and optical-electronic devices are carries out by laboratory staff: . ... Lens: . ... In the layout 1 prism systems perform functions of dispersive element, corrector of aberrations, optical reducer. ... Spectral range 200 - 400 nm; . ... Back Forward . ... The main corrector's function are compensation of field aberrations of the main spherical mirror of a telescope (diameter of 600 mm, f'=1200 mm) and increase aperture ratio. ...

Еще в разделе: (Показать все результаты (>659) - www.mao.kiev.ua/ )

• Achievements - Page 4

... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...

Еще в разделе: (Показать все результаты (>9074) - www.arcetri.astro.it/ )

• Arcetri Solar Physics Group: Solar Polarimetry
• LASG - Distribution specific information
• The Arcetri Spectral Code - E.Landi and M.Landini (2001)