... 1996 ]) and the SEDs in spectra of stars and YSOs (see Table 7 in Voshchinnikov ... chose a four-component mixture to explain observations of the young star HL Tau ... can be used rather for illustrative than for mass calculations (e.g., Wolff et al ...
... Though the single mechanism initiating the wind from evolved stars is not acknowledged yet, it is generally accepted that the mass loss is controlled by radiation pressure on dust grains (Lafon & Berruyer 1991; Winters 1994). ...
... distributions of classical Be stars" . Yudin R.V. A&A, 2001, v.368, p.912-931 . 2. ... 6. "On the Radio Emitting High Mass X--ray Binary LS 5039" . ... 15. "Polarimetry of evolved stars. I. RS CVn and Mira variables" . ...
... Scale height varies strongly with stellar type: z0 100 pc for young stars, z0 400 pc for older stars. ... mass of a galaxy, R is the characteristic radius (e.g. optical radius), G is the gravitational constant, and is a structural ...
... Tully et al. (1998) found dimming that was dependent on mass (luminosity) as well as on wavelength: CL (B ) = 1.57 + 2.75(lgW i ... 1 - 1.5, z stars /z dust 2 (V passband). ...
... Magnesium-aluminium spinel (MgAl 2 O 4 ) has been considered as a primary condensate in the outflows of oxygen-rich AGB stars and as a potential carrier of the 13 micron emission band observed in the spectra of these stars [ 10 ]. ...
... mass in the medium, the fluxes at wavelengths 100 are higher if the grains are ... stars (red giants and supergiants) and hotter stars, such as Herbig Ae/Be stars ... Star The temperature of particles of any shape decreases with distance from the ...
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