Photoevaporation of protoplanetary discs with PLUTO+PRIZMO - I. Lower X-ray–driven mass-loss rates due to enhanced cooling

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Volume 690 (October 2024)

A&A, 690 (2024) A296

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Table 3

Parameters derived for the fit to the mass-loss profile.

Fit parameter	Value
${\dot{M}}_{t o t}$ $\[\dot{M}_{\mathrm{tot}}\]$	4.3178 × 10⁻⁹ M_⊙ yr⁻¹
a	−1.2108
b	9.6815
c	−31.226
d	52.293
e	−48.475
f	25.093
g	−7.6443

${\dot{M}}_{f i t} (\leq 80 a u)$ $\[\dot{M}_{\mathrm{fit}}(\leq 80 ~\mathrm{au})\]$	1.50 × 10⁻⁹ M_⊙ yr⁻¹
${\dot{M}}_{true} (\leq 80 a u)$ $\[\dot{M}_{\text {true }}(\leq 80 ~\mathrm{au})\]$	1.06 × 10⁻⁹ M_⊙ yr⁻¹

Notes. The form of the profile is described by Eq. (15). The bottom two values give, for reference, the cumulative mass loss rate inside 80 au predicted from the fit and that measured directly in the simulation (as used in Sec. 5.2). We recommend using the full precision given here since the parameters are fits to exponents which can result in truncation errors compounding to give a poor fit at large radii.

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