EDP Sciences
Free Access
Issue
A&A
Volume 582, October 2015
Article Number A41
Number of page(s) 15
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201525966
Published online 02 October 2015

Online material

Appendix A: Snowline test

Water snowlines were inferred and compared with results from Min et al. (2011) in Fig. A.1 using the minimum mass solar nebula (MMSN) model (Σ ∝ r-1.5). The comparison shows that our adopted method reproduces the water snowlines at high accretion rates. For low accretion rates ≤ 10-9M yr-1, our values are slightly lower, but still consistent with those reported in literature.

thumbnail Fig. A.1

Snowlines for the MMSN disk without an envelope: black circles show the radii calculated with our method and red squares are tabulated values from Min et al. (2011).

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Appendix B: H2O, CO2, and CO gas fraction

The H2O, CO2 and CO gas pressure dependent gas fraction abundances are shown in Fig. B.1. Figures B.2 and B.3 show the midplane CO2 and CO snowlines as a function of luminosity and Rd similar to that of Fig. 9 for H2O.

thumbnail Fig. B.1

Gas fraction (ngas/ngas + nice) for H2O (top), CO2 (middle) and CO (bottom) as a function of density and temperatures.

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thumbnail Fig. B.2

Midplane CO2 snowline as a function of stellar luminosity, accretion rate, and disk radius. The parameters are similar to that of Fig. 9.

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thumbnail Fig. B.3

Midplane CO snowline as a function of stellar luminosity, accretion rate, and disk radius. The parameters are similar to that of Fig. 9.

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© ESO, 2015

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