Dust model for R coronae borealis and RY sagittarii

Krishna Swamy, K. S. (1972) Dust model for R coronae borealis and RY sagittarii Publications of the Astronomical Society of the Pacific, 84 (497). pp. 64-67. ISSN 0004-6280

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Official URL: http://www.jstor.org/pss/40675180


The observed infrared emission from R CrB and RY Sgr can be explained as due to thermal emission from the shell of dust grains surrounding these stars. We have calculated the emission spectrum of the dust shell as a function of the visual magnitude and also the expected flux of the star as a function of the optical depth of the dust shell. The question of the condensation of graphite particles in these stars is briefly discussed.

Item Type:Article
Source:Copyright of this article belongs to University of Chicago Press.
Keywords:Infrared Emission; Dust Grains; Carbon Stars
ID Code:87634
Deposited On:20 Mar 2012 14:33
Last Modified:20 Mar 2012 14:33

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