Titlebook: Light on Dark Matter; Proceedings of the F Frank P. Israel Conference proceedings 1986 D. Reidel Publishing Company, Dordrecht, Holland 198

橢圓

Submm Continuum Observations of Sources from the I R A S Point-Source CatalogueIR data and extensive model fits over this large spectral range allow the determination of the total luminosity, dust temperatures, the wavelength dependence of dust opacity, the total amount of extinction towards embedded stellar objects and the density distribution of dust around central heating s

rectocele

A Statistical Analysis of the LRS Catalogs types of spectra (LRS classes) can readily be associated with well-known groups of objects. About 96% of the sources are stars, most of them with oxygen- or carbon-rich envelopes, five sources are galaxies, and the others are compact HII regions, planetary nebulae, and ‘peculiar stars’.

騷動

The Zodiacal Background in the IRAS Datamicrometers. These data provide insights into the character, spatial distribution, and perhaps origin of these particles which both confirm and expand upon those gained from previous zodiacal light studies. The zodiacal emission is a major component of the large scale infrared brightness of the sky

RAFF

Heliocentric Dependences of Zodiacal Emission, Temperature and Albedo are retrieved from IRAS data (Hauser et al., 1984) in two localized regions of the line-of-sight, near 0.98 and 1.40 a.u. heliocentric distance. The model-dependence is reduced, compared to the values averaged on the line-of-sight. The temperature probably does not exceed 250 K at the distance of t

濃縮

噴出

鈍劍

Dust at the North Galactic Polemag. The reddened areas may be organized in parallel string-like features. The IRAS clouds B and C are located in the NGP zone and a reasonable agreement is obtained for the 100μ intensities estimated from the optical absorption observations and the infrared emission measurements. It is further indi

Angioplasty

努力趕上

執(zhí)拗

A Search for Infrared Excesses in G-Type Starsified, 15 have enhanced emission at λ > 25 μm. This group includes 4 supergiants, 8 variable stars, and 3 stars known to have dusty circumstellar medii (RU Cen, R Sge, HD-101584). The preliminary findings from this study are described.