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Accretion in Protoplanetary Disks: The Imprint of Core Properties

  • Authors: C. P. Dullemond, A. Natta, and L. Testi

Dullemond, Natta, & Testi 2006 The Astrophysical Journal Letters 645 L69.

  • Provider: AAS Journals

Caption: Fig. 1.

Mass accretion rate ﹩\dot{M}_{\mathrm{acc}\,}﹩ as function of the mass of the central object ﹩M_{*}﹩ in Taurus (left panel) and ρ Oph (right panel). Symbols are measured quantities or upper limits. Each line is a model series for fixed ω, as labeled, varying ﹩M_{\mathrm{core}\,}﹩. In all model series, ﹩\dot{M}_{\mathrm{infall}\,}﹩ and the snapshot time are kept constant (﹩10^{-5}\,M_{\odot }﹩ yr−1 and 1 Myr in Taurus and ﹩3\times 10^{-5}\,M_{\odot }﹩ yr−1 and 0.5 Myr in ρ Oph).

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