J/ApJS/214/25 Rosseland & Planck gaseous mean opacities (Freedman+, 2014)
Gaseous mean opacities for giant planet and ultracool dwarf atmospheres over a
range of metallicities and temperatures.
Freedman R.S., Lustig-Yaeger J., Fortney J.J., Lupu R.E., Marley M.S.,
Lodders K.
<Astrophys. J. Suppl. Ser., 214, 25 (2014)>
=2014ApJS..214...25F 2014ApJS..214...25F
ADC_Keywords: Models, atmosphere ; Abundances
Keywords: brown dwarfs; opacity; planets and satellites: atmospheres;
radiative transfer; stars: atmospheres
Abstract:
We present new calculations of Rosseland and Planck gaseous mean
opacities relevant to the atmospheres of giant planets and ultracool
dwarfs. Such calculations are used in modeling the atmospheres,
interiors, formation, and evolution of these objects. Our calculations
are an expansion of those presented in Freedman (2008ApJS..174..504F 2008ApJS..174..504F)
to include lower pressures, finer temperature resolution, and also the
higher metallicities most relevant for giant planet atmospheres.
Calculations span 1µbar to 300bar, and 75-4000K, in a nearly square
grid. Opacities at metallicities from solar to 50 times solar
abundances are calculated. We also provide an analytic fit to the
Rosseland mean opacities over the grid in pressure, temperature, and
metallicity. In addition to computing mean opacities at these local
temperatures, we also calculate them with weighting functions up to
7000K, to simulate the mean opacities for incident stellar
intensities, rather than locally thermally emitted intensities. The
chemical equilibrium calculations account for the settling of
condensates in a gravitational field and are applicable to cloud-free
giant planet and ultracool dwarf atmospheres, but not circumstellar
disks. We provide our extensive opacity tables for public use.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 153 1060 Mean Opacities for [M/H]=0.0
table4.dat 153 1060 Mean Opacities for [M/H]=0.5
table5.dat 153 1060 Mean Opacities for [M/H]=0.7
table6.dat 153 1060 Mean Opacities for [M/H]=1.0
table7.dat 153 1060 Mean Opacities for [M/H]=1.5
table8.dat 153 1060 Mean Opacities for [M/H]=1.7
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See also:
VI/133 : A variationally computed hot NH3 line list - BYTe (Yurchenko+, 2011)
J/A+A/562/A133 : Analytical model for atmospheres (Parmentier+, 2014)
J/MNRAS/440/1649 : ExoMol line lists for CH4 (Yurchenko+, 2014)
J/ApJS/210/21 : Refractive indices of grain materials (Cuzzi+, 2014)
J/A+A/494/403 : Low temperature Rosseland opacities (Lederer+, 2009)
J/ApJ/382/636 : Rosseland mean free-free Gaunt factor (Itoh+ 1991)
http://www.cfa.harvard.edu/hitran/updates.html : HITRAN database
http://ether.ipsl.jussieu.fr/etherTypo/?id=950 : GEISA database
Byte-by-byte Description of file: table[3-8].dat
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Bytes Format Units Label Explanations
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1- 4 I4 K T [75/4000] Gas local temperature (planet)
6- 10 E5.1 dPa P [1/3e+08] Gas pressure (dyne/cm2=dPa=µbar)
12- 21 E10.5 g/cm-3 rho [0/0.04] Gas density ρ
23- 32 E10.5 cm+2/g OpR Rosseland mean opacity κR(T,P,ρ) (1)
34- 43 E10.5 cm+2/g OpP Planck mean opacity κP(T,P,ρ) (1)
45- 54 E10.5 cm+2/g OpR3k Rosseland mean opacity κR using 3000K
stellar weighting function (1)
56- 65 E10.5 cm+2/g OpP3k Planck mean opacity κP using 3000K
stellar weighting function (1)
67- 76 E10.5 cm+2/g OpR4k Rosseland mean opacity κR using 4000K
stellar weighting function (1)
78- 87 E10.5 cm+2/g OpP4k Planck mean opacity κP using 4000K
stellar weighting function (1)
89- 98 E10.5 cm+2/g OpR5k Rosseland mean opacity κR using 5000K
stellar weighting function (1)
100-109 E10.5 cm+2/g OpP5k Planck mean opacity κP using 5000K
stellar weighting function (1)
111-120 E10.5 cm+2/g OpR6k Rosseland mean opacity κR using 6000K
stellar weighting function (1)
122-131 E10.5 cm+2/g OpP6k Planck mean opacity κP using 6000K
stellar weighting function (1)
133-142 E10.5 cm+2/g OpR7k Rosseland mean opacity κR using 7000K
stellar weighting function (1)
144-153 E10.5 cm+2/g OpP7k Planck mean opacity κP using 7000K
stellar weighting function (1)
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Note (1): the mean opacity is computed from monochromatic opacities with:
κP = ∫(κνB(T,ν)dν)/∫B(T,ν)dν
1/κR = ∫(1/κν)W(T,ν)dν/∫W(T,ν)dν
B(T,ν) = Planck function
W(T,ν) = dB(T,ν)/dT
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 15-Oct-2014