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Weighing protoplanetary discs with kinematics: physical model, method and benchmark
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abstract
The mass of protoplanetary discs sets the amount of material available for planet formation, determines the level of coupling between gas and dust, and possibly sets gravitational instabilities. Measuring mass of discs is challenging, since it is not possible to directly detect H$_2$, and CO-based estimates remain poorly constrained. An alternative method that does not rely on tracers-to-H$_2$ ratios has recently been proposed to dynamically measure the disc mass altogether with the star mass and the disc critical radius by looking at deviations from Keplerian rotation induced by the self-gravity of the disc. So far, this method has been applied to weigh three protoplanetary discs: Elias 2-27, IM Lup and GM Aurigae. We provide here a numerical benchmark of the method by simulating isothermal self-gravitating discs with a range of masses from 0.01 to $0.2 \,M_{\odot}$ with the phantom code and post-process them with radiative transfer (mcfost) to obtain synthetic observations. We find that dynamical weighing allows to retrieve the expected value of disc masses as long as the disc-to-star mass ratio is larger than $M_d/M_\star=0.05$. The estimated uncertainty for the disc mass measurement is $\sim 25\%$.
Forward citations
Cited by 5 Pith papers
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exoALMA. VI. Rotating under Pressure: Rotation curves, azimuthal velocity substructures, and pressure variations
Rotation-curve measurements of 15 protoplanetary disks show that the majority of dust rings and gaps sit at gas pressure maxima and minima, supporting pressure-driven dust trapping.
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exoALMA XII: Weighing and sizing exoALMA disks with rotation curve modelling
Modeling rotation curves of CO gas in ten exoALMA disks yields dynamical disk masses, scale radii, and effective viscosities, plus a gas-to-dust ratio around 400.
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exoALMA I. Science Goals, Project Design and Data Products
The exoALMA survey obtained deep, high-resolution ALMA images of 15 protoplanetary disks and found gas and dust substructure in 14 of them, along with small velocity disturbances in all sources.
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Extending dynamical mass measurements: probing GI as a possible origin of mm-dust spirals
Dynamical rotation-curve fits give M_disk ≈ 0.30 M_sun for HD 97048 and ≈ 0.21 M_sun for WaOph 6, and indicate disks with mm-dust spirals have systematically lower Toomre Q.
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exoALMA. XVIII. Interpreting large scale kinematic structures as moderate warping
Moderate disk warps of about 0.5 to 2 degrees can reproduce the single-armed velocity patterns seen in many exoALMA disks, and may also explain spiral structures in scattered light and CO temperature.
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