Fig. 6 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. 6.

Shu77 models for B335. Three models are shown: ﹩r_{\mathrm{inf}\,}=6200﹩ AU and ﹩s_{\mathrm{ISRF}\,}=1.0﹩, ﹩r_{\mathrm{inf}\,}=1000﹩ AU and ﹩s_{\mathrm{ISRF}\,}=1.0﹩, and ﹩r_{\mathrm{inf}\,}=1000﹩ AU and ﹩s_{\mathrm{ISRF}\,}=0.3﹩. The smaller infall radius of 1000 AU is a better fit than the best fit from Choi et al. (1995).

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