Understanding JWST water spectra: What can thermochemical models tell us about the (cold) water in protoplanetary disks?

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Table A.2

Summary of model grids and parameters.

Parameter	Symbol	Value
Disk structure - all models
Sublimation radius	R_subl	0.08 au
Outer radius	R_out	100 au
Characteristic radius	R_c	46 au
Characteristic gas surface density	Σ_c	21.32 g cm⁻²
Power-law index	γ	0.9
Characteristic scale height	h_c	0.08
Flaring index	ψ	0.11
Large dust mass fraction	f_ℓ	[0.9, 0.99, 0.999]
Large dust settling parameter	χ	0.2
Stellar parameters - chem. & param. models
Input stellar spectrum	-	AS 209^a
Stellar luminosity	L_*	1.4 L_⊙
Effective temperature	T_eff	4300 K
FUV luminosity	log L_FUV/L_⊙	−2.12
Stellar parameters - FUV models
Input stellar spectrum	-	4000 K blackbody +10 000 K excess^b
Stellar luminosity	L_*	0.8 L_⊙
Accretion luminosity	L_acc	[0, 0.002, 0.02, 0.2] L_⊙
Mass accretion rate	${\dot{M}}_{acc}$ $\[\dot{M}_{\text {acc}}\]$	[0, 10⁻¹⁰, 10⁻⁹, 10⁻⁸] M_⊙ yr⁻¹
FUV luminosity	log L_FUV/L_⊙	[−4.68, −3.75, −2.82, −1.82]
Elemental abundances - chem. & FUV models
C abundance	C/H	1.35 × 10⁻⁴
O abundance	O/H	2.88 × 10⁻⁴
Parameterized abundances - param. models
H₂O abundance - inner reservoir^c	n(H₂O)/n_H	10⁻⁴
H₂O abundance - outer reservoir^c	n(H₂O)/n_H	[10⁻⁶, 10⁻⁵, 10⁻⁴]
CO₂ abundance - upper reservoir^d	n(CO₂)/n_H	10⁻⁷
CO₂ abundance - lower reservoir^d	n(CO₂)/n_H	5 × 10⁻⁵

Notes. We divide the model parameters into categories, and we indicate which models these parameters apply to. The disk structure is kept consistent between all models presented in this work. We highlight in boldface the fiducial f_ℓ value of 0.9 (models with the other values are presented in Sect. A.3 and Fig. 6). All models except those presented in Sect. 4.1 (the "FUV" models) use the AS 209 spectrum as the input stellar spectrum. The FUV models instead use a blackbody with UV excess scaled to the mass accretion rate. ^(a) Zhang et al. (2021) ^(b) See Kama et al. (2016); Visser et al. (2018) ^(c) See Sect. 2 ^(d) See Sect. A.1

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