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J/A+A/539/A102      HD 209458 and HD 189733 theoretical spectra  (Hayek+, 2012)

Limb darkening laws for two exoplanet host stars derived from 3D stellar model atmospheres. Comparison with 1D models and HST light curve observations. Hayek W., Sing D., Pont F., Asplund M. <Astron. Astrophys. 539, A102 (2012)> =2012A&A...539A.102H
ADC_Keywords: Stars, G-type ; Stars, K-type ; Planets ; Spectroscopy Keywords: stars: atmospheres - stars: individual: HD 209458 - stars: individual: HD 189733 - planets and satellites: individual: HD 209458b planets and satellites: individual: HD 189733b Abstract: We compare limb darkening laws derived from 3D hydrodynamical model atmospheres and 1D hydrostatic MARCS models for the host stars of two well-studied transiting exoplanet systems, the late-type dwarfs HD 209458 and HD 189733. The surface brightness distribution of the stellar disks is calculated for a wide spectral range using 3D LTE spectrum formation and opacity sampling. We test our theoretical predictions using least-squares fits of model light curves to wavelength-integrated primary eclipses that were observed with the Hubble Space Telescope (HST). Description: Theoretical spectrum computations for the G-type dwarf HD 209458 and the K-type dwarf HD 189733 are presented, based on 3D hydrodynamical models of the stellar atmospheres. Surface intensities were computed in LTE using the SCATE spectrum formation code and cover the wavelength region between about 910 Angstroem and 20 micron with constant sampling of R=λ/δ_λ=20,000. The stellar disk was sampled at the disk center (µ=cos(θ)=1.0) and at angles µ = 0.90, 0.80, 0.70, 0.60, 0.50, 0.40, 0.30, 0.25, 0.20, 0.15, 0.125, 0.1, 0.075, 0.05, 0.025, 0.01 towards the limb. Use integration weights 0.05, 0.1, 0.1, 0.1, 0.1, 0.1, 0.1, 0.075, 0.05, 0.05, 0.0375, 0.025, 0.025, 0.025, 0.025, 0.02, 0.0125 to obtain fluxes. Objects: ---------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------- 20 00 43.7 +22 42 39 HD 189733 = HD 189733 22 03 10.8 +18 53 04 HD 209458 = V* V376 Peg ---------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file hd189733.dat 34 1833535 HD 189733 intensities hd209458.dat 34 1833535 HD 209458 intensities
See also: J/A+A/510/A21 : Stellar Limb-Darkening Coefficients (Sing, 2010) J/A+A/526/A71 : C abundances in G and K nearby stars (Da Silva+, 2011) J/A+A/529/A75 : Limb-darkening coefficients (Claret+, 2011) Byte-by-byte Description of file: hd189733.dat hd209458.dat
Bytes Format Units Label Explanations
1- 5 F5.3 --- mu [0.01/1] µ angle (1) 7- 18 E12.6 0.1nm lambda Vacuum wavelength 23- 34 E12.6 10-2W/m2/nm/sr Int Specific intensity (in erg/cm2/s/Å/sr)
Note (1): µ values are 0.010, 0.025, 0.075, 0.100, 0.125, 0.150, 0.200, 0.250, 0.300, 0.400, 0.500, 0.600, 0.7800, 0.800, 0.900 and 1.000.
Acknowledgements: Wolfgang Hayek, hayek(at)MPA-Garching.MPG.DE
(End) Wolfgang Hayek [MPA, Garching], Patricia Vannier [CDS] 03-Feb-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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