Rosseland and Planck mean opacities for protoplanetary discs

By D. Semenov, Th. Henning, Christiane Helling, M. Ilgner, E. Sedlmayr. 2003

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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 ∼1500 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 gc m −3 to 10 −7 gc m −3 . 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.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/413db91b0621d1a7f51d1344b089313620da0fd4

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Citations in the corpus

Global Models for the Evolution of Embedded, Accreting Protostellar Disks (2007, methodology): “The viscous dissipation per unit area is Fv = 3ṀΩ 8π , (19) and we compute the opacities using the Semenov et al. (2003) model for κR,P (T ): in particular, we use their homogeneous-aggregate dust model with normal silicates, calculated at the appropriate density.”
The birth of a galaxy – II. The role of radiation pressure (2012, background): “Above 1500 K, even the most stable dust species are sublimated and the Rosseland opacity drops by a few orders of magnitude (Semenov et al. 2003).”
UNLEASHING POSITIVE FEEDBACK: LINKING THE RATES OF STAR FORMATION, SUPERMASSIVE BLACK HOLE ACCRETION, AND OUTFLOWS IN DISTANT GALAXIES (2013, methodology): “I adopt a dust opacity at T 200 K given by the Rosseland mean opacity that depends only on temperature, scaling approximately as κ = κ0(T/T0)β, (13) where κ0T −2 0 = 2.4 × 10−4 cm2 g−1 K−2, and is valid at T T0 ≡ 100 K (Semenov et al. 2003).”
Fragmentation of massive protostellar discs (2006, background): “Tan & McKee 2004) By adopting the (relatively opaque) Semenov et al. (2003) dust opacities, we have underestimated disk fragmentation.”
THE DISRUPTION OF GIANT MOLECULAR CLOUDS BY RADIATION PRESSURE & THE EFFICIENCY OF STAR FORMATION IN GALAXIES (2009, methodology): “GivenT andρ, we use the opacity tables of Semenov et al. (2003) to find the Rosseland mean opacity in the outermost slice of the shell.”
The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity (2018, methodology): “In order to determine the opacities as a function of temperature, we fit a polynomial to the Semenov et al. (2003) opacities in the range of 10–400 K and adopt a constant value of κ=9.5 cm2 g−1 above >400 K for solar metallicity.”
Discovery of the Dust-Enshrouded Progenitor of SN 2008S with Spitzer (2008, neutral): “Setting τλ ≈ 1 ≈ κλρRBB, and assuming ρ = M/(4πR3BB/3), we find that M ∼ 10 −3κ−1λ, 10 M⊙, where κλ, 10 = κλ/10 cm 2 g−1 is a typical value for the Rosseland-mean dust opacity for gas at ∼ 440 K (e.g., Semenov et al. 2003).”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, methodology): “34 We take κeff for dust (T < 1500) from the detailed tables in Semenov et al. (2003), assuming the dust, gas, and radiative temperatures are in equilibrium (true in the optically thick limit at these temperatures), which is approximately well-fit by κeff = 5 for 150≤ T ≤ 1500 and κeff = 0.0027T…”
The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites (2017, background): “The opacity of the disk was set to a uniform value κ = 5 cm2 g−1, in the middle of the range of values calculated by Semenov et al. (2003).”
THE RUNTS OF THE LITTER: WHY PLANETS FORMED THROUGH GRAVITATIONAL INSTABILITY CAN ONLY BE FAILED BINARY STARS (2009, methodology): “For our fiducial model we use κ2 ≈ 5×10−4cm2/g for T in Kelvin, a fit to the standard dust model by Semenov et al. (2003).”
DIRECT NUMERICAL SIMULATION OF RADIATION PRESSURE-DRIVEN TURBULENCE AND WINDS IN STAR CLUSTERS AND GALACTIC DISKS (2012, methodology): “Choice of Simulation Parameters In all simulations we adopt an opacity law κ(R,P ) = (10 −3/2, 10−1) ( T 10K )2 cm2 g−1, (35) which is roughly in accord with the model of Semenov et al. (2003) at temperatures .”
Gravitational Instabilities in Circumstellar Disks (2016, background): “Semenov et al. (2003) find that the Rosseland mean opacity for small grains is well fit by κ2 ≈ 5× 10−4cm2/g.”
CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK (2012, background): “Optical constants for astrophysical grain components were obtained from Semenov et al. (2003), Zubko et al. (1996), and Warren (1984).”
THE PHYSICS OF THE FAR-INFRARED–RADIO CORRELATION. I. CALORIMETRY, CONSPIRACY, AND IMPLICATIONS (2009, background): “For parameters typical of starbursts and ULIRGs, κFIR ≈ 1−10 cm2 g−1 for Galactic dust-to-gas ratio and solar metallicity (Semenov et al. 2003).”
Origin and loss of nebula-captured hydrogen envelopes from ‘sub’- to ‘super-Earths’ in the habitable zone of Sun-like stars (2014, methodology): “For the gas and dust opacity we used tables from Freedman et al. (2008), and Semenov et al. (2003), respectively; for the equation of state we adopted the results of Saumon et al. (1995).”
Dynamics of Protoplanetary Disks (2010, background): “For an opacity appropriate for ice grains, for example, κ = κ0T 2 (Semenov et al. 2003), and Ωfrag ∝ κ −1/3 0 (Matzner & Levin 2005, Rafikov 2009).”
Radiation Pressure-supported Starburst Disks and Active Galactic Nucleus Fueling (2005, methodology): “Opacity Dependence Figure 1 shows the Rosseland mean opacity as a function of temperature for several densities using the publicly available opacities of Semenov et al. (2003) and Bell & Lin (1994).”
RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: PROTOSTELLAR CORE FORMATION (2012, methodology): “The dust opacities of Semenov et al. (2003) cover 10−18 < ρ (g cm−3) < 10−7.”