Hydrodynamic Photoevaporation of Protoplanetary Disks with Consistent Thermochemistry

Abstract

Photoevaporation is an important dispersal mechanism for protoplanetary disks. We conduct hydrodynamic simulations coupled with ray-tracing radiative transfer and consistent thermochemistry to study photoevaporative winds driven by ultraviolet and X-ray radiation from the host star. Most models have a three-layer structure: a cold midplane, warm intermediate layer, and hot wind, the last having typical speeds $\sim 30{\mathrm{km}\mathrm{s}}^{-1}$ and mass-loss rates $\sim 10^{-9}{M}_{\odot }{\mathrm{yr}}^{-1}$ when driven primarily by ionizing UV radiation. Observable molecules including CO, OH and H2O re-form in the intermediate layer and survive at relatively high wind temperatures due to reactions being out of equilibrium. Mass-loss rates are sensitive to the intensity of radiation in energy bands that interact directly with hydrogen. Comparison with previous works shows that mass loss rates are also sensitive to the treatment of both the hydrodynamics and the thermochemistry. Divergent results concerning the efficiency of X-ray photoevaporation are traced in part to differing assumptions about dust and other coolants.

15 pages, 9 figures, submitted to ApJ

References in corpus (9)

• Photoevaporation of protoplanetary discs II: evolutionary models and observable properties
• Photoevaporation of protoplanetary discs I: hydrodynamic models
• Heat and Dust in Active Layers of Protostellar Disks
• X-ray irradiated protoplanetary disk atmospheres I: Predicted emission line spectrum and photoevaporation
• Line Emission from Gas in Optically Thick Dust Disks around Young Stars
• Tracing Slow Winds from T Tauri Stars via Low Velocity Forbidden Line Emission
• Spatially extended PAHs in circumstellar disks around T Tauri and Herbig Ae stars
• Shielding by Water and OH in FUV and X-ray Irradiated Protoplanetary Disks
• Photochemical-dynamical models of externally FUV irradiated protoplanetary discs

Cited by in corpus (35)

• Global Hydromagnetic Simulations of Protoplanetary Disks with Stellar Irradiation and Simplified Thermochemistry
• The dispersal of protoplanetary discs. II: Photoevaporation models with observationally derived irradiating spectra
• The first multi-dimensional view of mass loss from externally FUV irradiated protoplanetary discs
• Photoevaporative Dispersal of Protoplanetary Disks around Evolving Intermediate-mass Stars
• A dusty origin for the correlation between protoplanetary disc accretion rates and dust masses
• JWST/NIRSpec Reveals the Nested Morphology of Disk Winds from Young Stars
• Radiation pressure clear-out of dusty photoevaporating discs
• Radiation hydrodynamics simulations of protoplanetary disks: Stellar mass dependence of the disk photoevaporation rate
• Modeling the CO outflow in DG Tau B: Swept-up shells versus perturbed MHD disk wind
• Radiation-Hydrodynamical Models of X-ray Photoevaporation in Carbon Depleted Circumstellar Discs
• Photoevaporation of protoplanetary discs with PLUTO+PRIZMO I. Lower X-ray-driven mass-loss rates due to enhanced cooling
• Disc population synthesis: Decrease in the solid mass reservoir through pebble drift
• High-resolution [O I] line spectral mapping of TW Hya supportive of a magnetothermal wind
• Forbidden line diagnostics of photoevaporative disc winds
• Three-temperature radiation hydrodynamics with PLUTO: Tests and applications to protoplanetary disks
• [OI] 6300Å emission as a probe of external photoevaporation of protoplanetary discs
• 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
• Migrating Low-Mass Planets in Inviscid Dusty Protoplanetary Discs
• Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
• Chemical network reduction in protoplanetary disks
• The Radial Distribution and Excitation of H2 around Young Stars in the HST-ULLYSES Survey
• The general applicability of self-similar solutions for thermal disc winds
• Giant planet migration during the disc dispersal phase
• Modelling thermochemical processes in protoplanetary disks I: numerical methods
• Time-dependent long-term hydrodynamic simulations of the inner protoplanetary disk III: The influence of photoevaporation
• Chandra Observations of Six Peter Pan Disks: Diversity of X-ray-driven Internal Photoevaporation Rates Doesn't Explain Their Rare Longevity
• Photoevaporation Can Reproduce Extended ${\mathrm{H}}_2$ Emission from Protoplanetary Disks Imaged by JWST MIRI
• The effect of stellar evolution on dispersal of protoplanetary disks: Disk fraction in star-forming regions
• The role of detailed gas and dust opacities in shaping the evolution of the inner disc edge subject to episodic accretion
• Long-term evolution of the temperature structure in magnetized protoplanetary disks and its implication for the dichotomy of planetary composition
• exoALMA XXI: The Morphology and Dynamics of Vertical Flows
• Formation of ring-like structures in flared α-discs with X-ray/FUV photoevaporation
• Photoevaporation from Inner Protoplanetary Disks Confronted with Observations
• Dispersal of protoplanetary discs: How stellar properties and the local environment determine the pathway of evolution