Far-ultraviolet and X-ray irradiated protoplanetary disks: a grid of models - I. The disk structure

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Issue		A&A Volume 547, November 2012


Article Number		A68
Number of page(s)		20
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201219863
Published online		01 November 2012

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Appendix B: Additional figures

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Fig. B.1

Main heating sources throughout the disk: FUV luminosity increasing from L_FUV = 10²⁹ (left) to 10³² erg/s. X-ray luminosity increasing from L_x = 0 to 10³² erg/s. background heating by [CII] (blue), PAH heating (orange), photo-electric heating (dark purple), X-ray Coulomb heating (light red), heating by collisional de-exciation of H₂ (blue-green), CI ionization heating (green-blue), infrared background by CO ro-vibrational lines (black), heating by thermal accomodation grains (white), cosmic ray heating (red), X-ray H₂ dissociation heating (light blue), free-free absorption (green), background heating by FeII (light green), background heating by SiII (green-yellow), infrared background heating by H₂O rotational transitions (yellow), heating by H₂ formation on dust (dark blue), and background heating by [OI] (purple).

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Fig. B.2

Main cooling sources throughout the disk: FUV luminosity increasing from L_FUV = 10²⁹ (left) to 10³² erg/s. X-ray luminosity increasing from L_x = 0 to 10³² erg/s. Lyman α cooling (black), [FeII] line cooling (blue-green), [OI] line cooling (white), [CII] line cooling (yellow), CO rotational and ro-vibrational cooling (red), H₂O rotational cooling (green-blue), OH rotational cooling (light green), HCN line cooling (dark purple), [CI] line cooling (light purple), HNC line cooling (blue), cooling by thermal accomodation on grains (dark blue), CS line cooling (yellow-green), H₂ line cooling (light blue), chemical cooling (red-orange), and free-free emission (green).

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	Fig. B.3 Electron abundance: FUV luminosity increasing from L_FUV = 10²⁹ (left) to 10³² erg/s (right). X-ray luminosity increasing from L_x = 0 (top) to 10³² erg/s (bottom).
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	Fig. B.4 H abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.5 H₂ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.6 H⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.7 H⁻ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.8 H abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.9 H abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.10 C²⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.11 C⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.12 C abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.13 CO abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.14 O²⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.15 O⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.16 O abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.17 OH abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.18 H₂O abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.19 OH⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.20 H₂O⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.21 H₃O⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.22 Ne⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.23 Ne²⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.24 Ar⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.25 Ar²⁺ abundances. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.26 Radial column density distribution of C⁺. FUV and X-ray fluxes are the same as Fig. B.3.
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	Fig. B.27 Radial column density distribution of Ne²⁺. FUV and X-ray fluxes are the same as Fig. B.3.
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© ESO, 2012

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