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

Abstract

Context: Photoevaporation is an important process for protoplanetary disc dispersal but there has so far been a lack of consensus from simulations over the mass-loss rates and the most important part of the high-energy spectrum for driving the wind. Aims: We aim to isolate the origins of these discrepancies through carefully-benchmarked hydrodynamic simulations of X-ray photoevaporation with time-dependent thermochemistry calculated on the fly. Methods: We conduct hydrodynamic simulations with pluto where the thermochemistry is calculated using prizmo. We explore the contribution of certain key microphysical processes and the impact of using different spectra used previously in literature studies. Results: We find that additional cooling results from the excitation of O by neutral H, which leads to dramatically reduced mass-loss across the disc compared to previous X-ray photoevaporation models, with an integrated rate of 10^-9 Msun/yr. Such rates would allow for longer-lived discs than previously expected from population synthesis. An alternative spectrum with less soft X-ray produces mass-loss rates around a factor of 2-3 times lower. The chemistry is significantly out of equilibrium, with the survival of H2 into the wind aided by advection. This leads to its role as the dominant coolant at 10s au - thus stabilising a larger radial temperature gradient across the wind - as well as providing a possible wind tracer.

26 pages, 16 figures, Accepted 31st July 2024 for publication in A&A

References in corpus (38)

• PLUTO: a Numerical Code for Computational Astrophysics
• Monte Carlo radiative transfer in protoplanetary disks
• Evolution of interstellar dust and stardust in the solar neighbourhood
• Uncertainties in H2 and HD Chemistry and Cooling and their Role in Early Structure Formation
• Global Simulations of the Inner Regions of Protoplanetary Disks with Comprehensive Disk Microphysics
• Star formation at very low metallicity. I: Chemistry and cooling at low densities
• Photodissociation and X-Ray Dominated Regions
• The Impact of Dust Evolution and Photoevaporation on Disk Dispersal
• Images of Embedded Jovian Planet Formation At A Wide Separation Around AB Aurigae
• Neon Fine-Structure Line Emission By X-ray Irradiated Protoplanetary Disks
• X-ray enabled MOCASSIN: a 3D code for photoionized media
• Non-equilibrium chemistry and cooling in the diffuse interstellar medium - II. Shielded gas
• Consistent dust and gas models for protoplanetary disks: II. Chemical networks and rates
• Global Hydromagnetic Simulations of Protoplanetary Disks with Stellar Irradiation and Simplified Thermochemistry
• Hydrodynamic Photoevaporation of Protoplanetary Disks with Consistent Thermochemistry
• Gas phase Elemental abundances in Molecular cloudS (GEMS) VII. Sulfur elemental abundance
• Confirmation and Keplerian motion of the gap-carving protoplanet HD 169142 b
• The dispersal of protoplanetary discs. II: Photoevaporation models with observationally derived irradiating spectra
• Blobs, spiral arms, and a possible planet around HD 169142
• Coronae and Winds from Irradiated Disks in X-ray binaries
• A dusty origin for the correlation between protoplanetary disc accretion rates and dust masses
• Thermal Disk Winds in X-ray Binaries: Realistic Heating and Cooling Rates Give Rise to Slow, but Massive Outflows
• Modeling the delivery of dust from discs to ionized winds
• Radiation hydrodynamics simulations of protoplanetary disks: Stellar mass dependence of the disk photoevaporation rate
• X-ray radiative transfer in protoplanetary disks - The role of dust and X-ray background fields
• Population study on MHD wind-driven disc evolution -- Confronting theory and observation
• Radiation-Hydrodynamical Models of X-ray Photoevaporation in Carbon Depleted Circumstellar Discs
• Effects of photoevaporation on protoplanetary disc `isochrones'
• Disc population synthesis: Decrease in the solid mass reservoir through pebble drift
• Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level
• Forbidden line diagnostics of photoevaporative disc winds
• Dust delivery and entrainment in photoevaporative winds
• The distribution of accretion rates as a diagnostic of protoplanetary disc evolution
• The importance of X-ray frequency in driving photoevaporative winds
• Interpreting molecular hydrogen and atomic oxygen line emission of T Tauri disks with photoevaporative disk-wind models
• Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
• Dust entrainment in photoevaporative winds: Synthetic observations of transition disks
• Modelling thermochemical processes in protoplanetary disks I: numerical methods

Cited by in corpus (13)

• There is no disk mass budget problem of planet formation
• Mapping Synthetic Observations to Prestellar Core Models: An Interpretable Machine Learning Approach
• Photoevaporation Can Reproduce Extended ${\mathrm{H}}_2$ Emission from Protoplanetary Disks Imaged by JWST MIRI
• Changing disc compositions via internal photoevaporation II: M dwarf systems
• On the diversification and dissipation of protoplanetary disks
• The role of detailed gas and dust opacities in shaping the evolution of the inner disc edge subject to episodic accretion
• exoALMA XXI: The Morphology and Dynamics of Vertical Flows
• The survivorship bias of protoplanetary disc populations
• Using simultaneous mass accretion and external photoevaporation rates for d203-504 to constrain disc evolution processes
• Effects of Stellar X-ray Photoevaporation on Planetesimal Formation via the Streaming Instability
• Line ratio identification of external photoevaporation
• Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
• Survival of Protoplanetary Disks in Upper Scorpius from Population Synthesis Models with External Photoevaporation