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861. Database of Optical Properties -- Level: subsubpage
Cross-sections and albedo for homogeneous spheroids . ... The dependence on the size parameter x for different refractive indices m=n+k i . ... Q abs (x) . albedo (x) . ... Parameters: n = 1.3; k = 0, 0.01, 0.03, 0.1, 0.3; x = 0--20. ... Notes: Q abs =0, albedo=1, when k=0. ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/BASICS/SPH/sph.html -- 7.9 Кб -- 19.11.2010
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862. Database of Optical Properties -- Level: subpage
... Links given for particles of different shapes allow one to access our graphics illustrating the dependence of various optical properties of model scatterers on their parameters. ... Q ext , Q sca , Q abs , Q bk , albedo, g, Q pr vs x for different m . ... Q ext , Q sca , Q abs , Q bk , albedo, g, Q pr vs x for different m core , m mantle , V core /V total . ... Q ext , Q sca , Q abs , albedo, Q pol vs x for different m, alpha . ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/BASICS/index.html -- 4.3 Кб -- 19.11.2010
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863. Database of Optical Properties -- Level: subsubpage
Cross-sections, albedo, asymmetry factor for core-mantle spheres . ... The dependence on the size parameter x for different ratio of core to total volume V core /V total . ... Parameters: V core /V total = 0, 0.25, 0.5, 0.75, 1; m mantle = 1.3; m core = 2.5+1.5i; x = 0--20 . ... The dependence on the size parameter x for different refractive index of the core m core . ... 1.3. The dependence on the size parameter x for different refractive index of the mantle m mantle . ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/BASICS/S_CM/s-cm.html -- 6.4 Кб -- 19.11.2010
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864. Linear polarization: wavelength dependence
... 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. ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node7.html -- 18.9 Кб -- 19.11.2010
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865. Polarization efficiency: size/shape/orientation effects
... The behaviour of the polarization efficiency (see Eq. ( 14 )) for non-absorbing and absorbing spheroids is shown in Fig. 11 for the case when a maximum polarization is expected (PF alignment, ). ... Figure 11: Polarization efficiency against for prolate and oblate spheroids with and , picket fence orientation, . The size/shape effects are illustrated. ... Figure: Polarization efficiency as a function of particle equivolume radius for prolate core-mantle spheroids with and , PF orientation, . ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node6.html -- 28.1 Кб -- 19.11.2010
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866. Footnotes
... Crystalline graphite has a strong resonant feature near 11.52 (Draine, [ 1984 ]) which is not observed... width 2 . Note that the observed weakness of the bump strength in dense clouds can be attributed to the hydrogenation of carbon (Sorrell, [ 1990 ]).. ... Its idea was first suggested by Gold ([ 1952 ])...fpell) 4 . A similar conclusion follows from calculations made by Matsumura and Seki ([ 1996 ])... ``correct'' 5 . ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/footnode.html -- 3.8 Кб -- 19.11.2010
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867. Polarization properties (transmitted radiation)
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 ( ). ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node5.html -- 24.1 Кб -- 19.11.2010
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868. Scattering properties
. Next: Absorption/emission properties Up: Optical properties of cosmic Previous: Circular polarization: change of . to be given . root 2003-04-09
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node9.html -- 2.9 Кб -- 19.11.2010
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869. About this document ...
Up: Optical properties of cosmic Previous: Bibliography . Optical properties of cosmic dust analogs . This document was generated using the LaTeX 2 HTML translator Version 2K.1beta (1.48) . Copyright © 1993, 1994, 1995, 1996, Nikos Drakos , Computer Based Learning Unit, University of Leeds. Copyright © 1997, 1998, 1999, Ross Moore , Mathematics Department, Macquarie University, Sydney. ... The translation was initiated by root on 2003-04-09 . root 2003-04-09 ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node12.html -- 3.4 Кб -- 19.11.2010
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870. The 2175? feature
... Laboratory and theoretical modelling of the UV bump on the interstellar extinction curve is a very popular topic in dusty investigations. ... feature is illustrated by Fig. 10 where the profiles were calculated using the model of graphite spheres. Figure 10: Normalized extinction efficiencies for graphite spheres. ... The lower panel shows the summary extinction of two graphite spheres with radii and (from upper panel) taken in equal proportions. ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node4.html -- 13.3 Кб -- 19.11.2010
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871. Optical properties of cosmic dust analogs
Next: Extinction properties (transmitted radiation) . ... The notes in their current form concern only 2 but main for astronimy aspects of the optical properties of cosmic dust - the ability to extinct and polarize transmitted radiation. The corresponding obervational effects the extinction and polarization (not due to scattering) plaied and plays till now the primary role in astrophysical effects of cosmic dust considered in the literature. ... Extinction properties (transmitted radiation) . ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/n6.html -- 4.9 Кб -- 19.11.2010
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872. Extinction properties (transmitted radiation)
Next: Extinction efficiencies: general behaviour Up: Optical properties of cosmic Previous: Optical properties of cosmic . It is now evident that observed interstellar extinction cannot be explain using particles of only one kind. ... The intensity of radiation after passing a dust cloud is equal to . ... The interstellar extinction is . ... Next: Extinction efficiencies: general behaviour Up: Optical properties of cosmic Previous: Optical properties of cosmic root 2003-04-09 ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node1.html -- 11.6 Кб -- 19.11.2010
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873. Bibliography
... 1979 . ... 1990 . Chlewicki, G. and Greenberg, J.M. (1990) Astrophys. ... Clayton, G.C. and Cardelli, J.A. (1988) Astron. ... 1996 . Draine, B.T. and Weingartner, J.C. (1996) Astrophys. ... Voshchinnikov, N.V. (1989) Astron. ... Voshchinnikov, N.V. (1990) Sov. ... Voshchinnikov, N.V. (1996) J. Quant. ... Voshchinnikov, N.V. (2002) Astrophys. ... Voshchinnikov, N.V. and Farafonov, V.G. (2002) Measurement Sci. and Technology , 13 , 249 . ... Voshchinnikov, N.V. and Mathis, J.S. (1999) Astrophys. ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node11.html -- 10.8 Кб -- 19.11.2010
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874. Circular polarization: change of sign
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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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node8.html -- 13.2 Кб -- 19.11.2010
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875. Absorption/emission properties
. Next: Bibliography Up: Optical properties of cosmic Previous: Scattering properties . to be given . root 2003-04-09
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node10.html -- 2.9 Кб -- 19.11.2010
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876. Wavelength dependence
... The first task assumes the searching for chemical composition and sizes of particles which give the wavelength dependence of the extinction efficiencies close to the observed dependence of . Figure 7: Wavelength dependence of the extinction efficiency factors for homogeneous spherical particles of different sizes consisting of astronomical silicate and amorphous carbon. The dashed segment shows the approximate wavelength dependence of the mean galactic extinction curve at optical wavelengths. ...
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node3.html -- 15.8 Кб -- 19.11.2010
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877. Extinction efficiencies: general behaviour and deviations
... The extinction efficiency factors are usually considered as a function of the size parameter for a fixed refractive index that, strictly speaking, does not characterize the dependence because of the wavelength dependence of (Sect. 2.1.2 in Voshchinnikov [ 2002 ]). ... This behaviour is typical for weakly absorbing homogeneous spheres (Fig. 1 , upper panel; see also Fig. 11 in Voshchinnikov [ 2002 ]). ... The deviations from it occur when the inhomogeneous or/and non-spherical particles are examined....
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Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node2.html -- 29.5 Кб -- 19.11.2010
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878. http://www.astro.spbu.ru/DOP/6-SOFT/SPHEROID/2-SPH/cm.nrm
CORE / MANTLE SPHEROID: Prolate Refractive index: 1.7000 0.0000i / 1.3000 0.0000i Lambda= 0.550 mkm, Rv= 0.041 / 0.088 mkm, Xv= 0.464 / 1.000, a/b= 5.24 / 2.00, ksi = 1.019 / 1.155, Volume: core / total= 0.10 .. C1= 1.37 C2= 1.79 0.00 C3= 2.34 0.00 Cksi= 1.59 Cksi2= 1.40 Nmax= 6 Nmxe= 14 ------------------------------------------------------------------------------ alpha m Cext/(Pi*Rv**2) Csca/(Pi*Rv**2) Cabs/(Pi*Rv**2) .. ...
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Ссылки http://www.astro.spbu.ru/DOP/6-SOFT/SPHEROID/2-SPH/cm.nrm -- 6.7 Кб -- 19.11.2010
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879. http://www.astro.spbu.ru/DOP/6-SOFT/SPHEROID/2-SPH/cm.res
CORE / MANTLE SPHEROID: Prolate Refractive index: 1.7000 0.0000i / 1.3000 0.0000i Lambda= 0.550 mkm, Rv= 0.041 / 0.088 mkm, Xv= 0.464 / 1.000, a/b= 5.24 / 2.00, ksi = 1.019 / 1.155, Volume: core / total= 0.10 .. ...
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Ссылки http://www.astro.spbu.ru/DOP/6-SOFT/SPHEROID/2-SPH/cm.res -- 6.9 Кб -- 19.11.2010
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880. Database of Optical Properties -- Level: subsubpage
... This page will present thoroughly checked optical properties in tabular form: . Fixed orientation, single particle . Data tables classified by shapes, m, a/b, orientation, etc. quantities . ... Q ext , Q sca , Q bk , g, some F ij . ... Q ext , Q sca , Q bk , g, ind (TE/TM) . inf.cyl. 20*x, 4*alpha, 10*m . ... fin.cyl. 10*x, 7*L/D, 4*alpha, 5*m . ... 10*x, 9*a/b, 4*alpha, 5*m . ... Chebyshev p. 10*x, 4*n, 6*eps, 4*alpha, 5*m . ... Random orientation, single particle . ...
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Ссылки http://www.astro.spbu.ru/DOP/7-BENC/OURS/index.html -- 3.3 Кб -- 19.11.2010
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