. 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

We model the spectral chanages of late oxygen-rich Miras observed in different pulsation phases. From a combination of variable near-IR spectra and UKIRT spectrophotometry of the 9.7 \mu m silicate dust emission feature in different phases we study the influence of the changing atmospherical circumstances on the conditions in the circumstellar dust shell. ... A comparision with the modelling results for another long period Mira U Ori is also provided. ...

... In the first page of this chapter, Eddington computes an effective temperature of 3.18 K, but this has nothing to do with the 2.725 K blackbody spectrum of the Cosmic Microwave Background (CMB) . Here is a quote of what Eddington actually said: . ... We shall first calculate the energy density of this radiation. ... It is clear that Eddington's model fits the optical data, but that Eddington did not anticipate either the CMB (red curve) or the interstellar dust (ISD, green curve). ...

. 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.

... arfgen (arfgen-1.75.6) [?? ... arfgen simply constructs the appropriate quantities from the CAL, in the form of vectors of discrete energy-dependent elements, and combines these data multiplicatively to form the ancilliary response. ... This is already taken into account by the CAL in the call to CAL_effectiveArea. The user can enable or disable the effective area, filter transmission, QE or grating attenuation by setting the relevant parameter (eg modeleffarea ) to true or false respectively. ...

... Posts tagged ?effective area? ... highlighting some equation that is widely used in astrophysics or astrostatistics. ... Tags: ARF , effective area , EotW , Equation , Equation of the Week , LRF , point spread function , PSF , response matrix , RMF , source . ... Comment . ... Entries RSS . Comments RSS . ... vlk on [MADS] Parallel Coordinates . upvc windows on [MADS] Parallel Coordinates . ... Alfred Inselberg on [MADS] Parallel Coordinates . ... Entries (RSS) and Comments (RSS) . ...

... Roland Buser has provided an extensive collection of Kurucz (1979) model atmosphere spectra covering a wide range in metallicity, effective temperature, and gravity. ... The BK atlas is a library of stellar flux spectra calculated by Kurucz and Buser from theoretical model atmospheres. ... For convenient use, the BK atlas flux spectra have been subdivided into separate blocks (or sub-atlases) corresponding to the physical distinctions of their underlying model atmospheres, as described above. ...

TOWARDS SUPERSENSITIVE BOLOMETERS AND ELECTRON COOLERS BASED ON CARBON NANOTUBES M.TARASOV, J.SVENSSON, S.DITTMER, L.KUZMIN, AND E.CAMPBELL Chalmers University of Technology, GЖteborg SE 41294, Sweden E-mail: Mikhail.tarasov@mc2.chalmers.se Carbon nanotubes (CNT) are being intensively developed for novel electronics. Electron cooling by superconductor-insulator-nanotube (SIN) tunnel junctions could be extremely effective due to the small volume of the CNT. ...

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

... Theoretical and experimental investigations electrodynamical characteristics of RATAN-600. Calculation of the two- and thee-mirror periscopic systems of RATAN-600 and optimization their characteristics. Measurements and calculation of the antenna noise temperature of the RATAN-600 radio telescope. ... Calculation and experimental investigation of the characteristics of the radio telescope RATAN-600 when the primary feed is shifted from the focus. ... The "radio-Schmidt telescope" mode. ...

Next: Antenna gain considerations and Up: Some theory Previous: Some theory . To provide correct flux density units for the visibilities, , from an interferometer, the measured correlation coefficient at the correlator ( ) needs to be scaled by a system temperature and a telescope sensitivity factor ( ). ... For a zenith opacity , observing at an elevation of , and if the atmosphere is approximated as having a uniform temperature , then the atmospheric contribution to system temperature is . ...

... Science . ... Other Science . ... I found that the attractive interaction between holes increases in strength as the system is moved towards the superconducting phase and that the curves of constant energy closely resemble those of a free particle. The results provide convincing evidence that the pairing mechanism results precisely from the hole interaction. Thesis available upon email request. Copyright 2007 Emma Kirby. ... All Photos were taken by Emma Kirby unless otherwise stated. ...

... 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. ...

... Spectroscopy of Semiconductors and Dielectrics . ... Interband optical transitions and their optical properties. ... Excitons in crystals. ... Collective interaction effects in exciton and nonequilibrium high-density carrier system. ... Carrier spin and exciton optical orientation in semiconductors. ... Two-dimensional excitons in quantum wells and related quantum systems. €аState density in transverse magnetic field and effect of random potential fluctuation on one-particle spectrum shape. ...

home education . SEARCH ASP SITE: Match ALL words Match ANY word . ... SEED Grants to Scientists . ... The ASP SEED Grant program supports the ASP's mission to advance science and science literacy through astronomy by encouraging active researchers to engage in public outreach, K-14 formal education, or informal education programs or activities. ... Development, use, and dissemination of a well-illustrated college-level presentation on a specific topic or problem in current research . ... search . ...

... Stellar magnitudes, provided by observations in an optical band, are reduced to the units of erg/cm /s as follows: . ... Table: `Zero-points', central wavelengths, and effective widths of optical bands (Zombeck's Handbook, 1990). - the corrected value (the handbook value is given in parentheses). ... We have achieved coincidence between theoretical values by Bochkarev et al (1991) and ours, obtained with rectangular shapes of transmission band of optical filters. ... 1991, V. 1, P. 41. ...

observed energy levels: Edlen, B., 1983, Phys. Scr., 28, 51 %theoretical energy levels: Butler, K., Zeippen, C.J., 1994, AASS, 108, 1. %produced as part of the Arcetri/Cambridge/NRL atomic data base collaboration CHIANTI and the Arcetri Spectral Code % Enrico Landi 1997 . ...

... BOT OF M2 CONE TOP OF M3 CONE M3 INT. BAF1 M3 INT. BAF2 M3 INT. BAF3 M3 INT. BAF4 M3 INT. BAF5 : Angle in degrees Y-Value Weight 0.000000 0.500000 0.050000 1.000000 0.075000 2.000000 0.090000 0.500000 0.099500 0.500000 VCX 0.000000 0.000000 0.000000 0.000000 0.000000 VCY 0.000000 0.000000 0.000000 0.000000 0.000000 VAN 0.000000 0.000000 0.000000 0.000000 ...

... 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. ...