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Rotation curves in protoplanetary disks with thermal stratification
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In recent years the gas kinematics probed by molecular lines detected with ALMA has opened a new window to study protoplanetary disks. High spatial and spectral resolution observations have revealed the complexity of protoplanetary disk structure and correctly interpreting these data allow us to gain a better comprehension of the planet formation process. We investigate the impact of thermal stratification on the azimuthal velocity of protoplanetary disks. High resolution gas observations are showing velocity differences between CO isotopologues, which cannot be adequately explained with vertically isothermal models. The aim of this work is to determine whether a stratified model can explain this discrepancy. We analytically solve the hydrostatic equilibrium for a stratified disk and we derive the azimuthal velocity. We test the model with SPH numerical simulations and then we use it to fit for star mass, disk mass and scale radius of the sources in the MAPS sample. In particular, we use 12CO and 13CO datacubes.
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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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Angular Momentum of Planet-Forming Disks: Implications for Infall Driven Misalignments
Most planet-forming disks have less angular momentum than late-infalling cloud gas is predicted to carry, so infalling streamers are a plausible cause of the observed misalignments.
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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): III. Dust and Gas Disk Properties in the Lupus Star-forming Region
Deep ALMA observations of 10 Lupus disks detect rare CO isotopologues and N2H+, revealing correlations between gas and dust fluxes and giving gas-to-dust mass ratios of 10 to 100.
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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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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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