Fig. 3 from Tracing the Mass during Low‐Mass Star Formation. III. Models of the Submillimeter Dust Continuum Emission from Class 0 Protostars

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Tracing the Mass during Low‐Mass Star Formation. III. Models of the Submillimeter Dust Continuum Emission from Class 0 Protostars

Authors: Yancy L. Shirley, Neal J. Evans II, and Jonathan M. C. Rawlings

Shirley, Evans, & Rawlings 2002 The Astrophysical Journal 575 337.

Provider: AAS Journals

Caption: Fig. 3.

B335 power‐law models with ﹩p=1.5﹩, 2.0, and 2.5. The ﹩p=2.0﹩ model is the best fit to the SED and radial profiles. The model parameters were OH5 dust opacities, ﹩s_{\mathrm{ISRF}\,}=1.0﹩, ﹩r_{i}=60﹩ AU, and ﹩r_{o}=60,000﹩AU for all models.

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