Rosseland and Planck Mean Opacities for Protoplanetary Discs

Abstract

In this paper, we present mean gas and dust opacities relevant to the physical conditions typical of protoplanetary discs. As the principal absorber for temperatures below ~1,500 K, we consider spherical and aggregate dust particles of various sizes, chemical structure, and porosity, consisting of ice, organics, troilite, silicates, and iron. For higher temperatures, ions, atoms, molecules, and electrons are included as the main opacity sources. Rosseland and Planck mean opacities are calculated for temperatures between 5 K and 10,000 K and gas densities ranging from 10^{-18} g/ccm to 10^{-7} g/ccm. The dependence on the adopted model of dust grains is investigated. We compare our results with recent opacity tables and show how different opacity models affect the calculated hydrodynamical structure of accretion discs.

12 pages, 4 figures, to be published in A&A, 2003

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• Two-Dimensional Radiation-Hydrodynamic Simulations of Luminous Red Novae
• Dynamics of magnetic flux tubes in accretion discs of T Tauri stars
• Self-Sustained Recycling in the Inner Dust Ring of Pre-Transitional Disks
• Photon Feedback: Screening and the Eddington Limit
• Effects of Chemistry on Vertical Dust Motion in Early Protoplanetary Disks
• Dust evolution by chemisputtering during protostellar formation
• Radiation Hydrodynamics Simulations of Spherical Protostellar Collapse for Very Low Mass Objects
• Planetary Accretion Shocks with a Realistic Equation of State
• Restoration of the Parameters of a Gas-Dust Disk Based on Its Synthetic Images
• Dynamics of magnetized accretion disks of young stars
• Simulations of the isothermal collapse of magnetic rotating protostellar clouds
• Ionization degree and magnetic diffusivity in star-forming clouds with different metallicities
• DIPSY: A new Disc Instability Population SYnthesis, I. Modeling, evolution of individual systems, and tests
• Formation of low-mass stars and brown dwarfs
• Monte Carlo post-processing for radiation hydro simulations of accreting planets in protoplanetary disks
• C/O ratios in self-gravitating protoplanetary discs with dust evolution
• The influence of dust growth on the observational properties of circumplanetary discs
• RAPOC : the Rosseland and Planck opacity converter. A user-friendly and fast opacity program for Python
• Formation of chondrules in radiative shock waves I. First results, spherical dust particles, stationary shocks
• Transit flow models for low and high mass protostars
• New constraints on the presence of debris disks around G 196-3 B and VHS J125601.92-125723.9 b
• From Common Envelope Evolution to Luminous Red Novae I: A One-dimensional Radiation Hydrodynamic Model
• A physical model for radiative, convective dusty disk in AGN
• The Compositional Dimension of Planet Formation
• Episodic accretion in high-mass star formation: An analysis of thermal instability for axially symmetric disks
• Modeling the Far-Infrared Polarization Spectrum of a High-Mass Star Forming Cloud
• Evolution and Observable Properties of Rocky Planet Atmospheres
• Volatile enrichment in low-mass planets: Signatures of past planetary disruption?
• Icy Volatile Enhancements in Evolving Protoplanetary Disks
• Modelling the Break in the Specific Angular Momentum within the Envelope-Disk Transition Zone
• Dust growth and planet formation by disc fragmentation
• When did the initial mass function become bottom-heavy?
• How two-dimensional are planet-disc interactions? II. Radiation hydrodynamics and suitable cooling prescriptions
• Radiative, magnetic and numerical feedbacks on small-scale fragmentation
• Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
• Evolution of Mercury's Earliest Atmosphere
• Planetary migration in wind-fed non-stationary accretion disks in binary systems
• A novel sub-grid model for super-Eddington accretion of spinning black holes in galaxy-scale simulations
• Protoplanetary disk formation from the collapse of a prestellar core
• Discs and outflows in the early phases of massive star formation: influence of magnetic fields and ambipolar diffusion