New Dimensions of Stellar Atmosphere Modelling Derek Homeier 1,2 France Allard 1,3 Bernd Freytag 1 1 CRAL/École Normale Supérieure de Lyon 2 Förderkreis Planetarium Göttingen e.v. 3 Institut d Astrophysique de Paris 8 th Serbian Conference on Spectral Line Shapes in Astrophysics Divčibare, Serbia 6-10 June 2011
(Sub-) stellar atmosphere modelling independent Variables (minimal): INPUT line opacity effective temperature T eff surface gravity g(r) = GM/r 2 mass M or radius R or luminosity L = 4 π R 2 4 σ T eff ITERATION Pressure Stratification Radiation Field OUTPUT continuum opacity molecular band opacity composition ( metallicity ) Converged? YES END SYNTHETIC SPECTRUM NO Temperature Correction PHOENIX workflow (P. Hauschildt)
(Sub-) stellar atmosphere modelling independent Variables (minimal): INPUT line opacity effective temperature T eff surface gravity g(r) = GM/r 2 mass M or radius R or luminosity L = 4 π R 2 4 σ T eff ITERATION Pressure Stratification Radiation Field OUTPUT continuum opacity molecular band opacity composition ( metallicity ) convection (micro-) turbulence & mixing rotation chemical peculiarities magnetic fields etc. Converged? Temperature Correction adding more dimensions to the modelling problem END SYNTHETIC SPECTRUM NO YES PHOENIX workflow (P. Hauschildt)
Model Spectra and Line Synthesis Solar disk-centre spectrum (blue) 3D RHD model with LTE spectrum (red dots) with fitted gf from Bigot & Thevenin 2008; PHOENIX 1D NLTE model (green), same gf, γvdw by Barklem et al. 2000
Atmosphere Models and Turbulence thin disk thick disk halo dsph galaxies α-element abundances from Venn et al. (2004) No unique relation between metallicity and α-enhancement between different populations or even within one population at least one additional dimension in chemical composition
Atmosphere Models and Turbulence Turbulent velocity from CO3BOLD 2D+3D RHD models (triangles) PHOENIX 1D models estimated from MLT (dashed lines) fitted to observed spectra of B F dwarfs by Landstreet et al. (2009, errorbars) and G K giants by Takeda et al. (2008, circles) 1D treatment of convection reproduces trends found in multi-d simulations and empirically fitted microturbulence Improvements in treatment of convective boundary required!
Spectral Shapes of Cool Atmospheres M-L-T-(Y?)-dwarfs 1e-10 VO TiO FeH CH 4 CO d = 5pc 1e-11 1e-12 K I H 2 O CH 4 CH 4 CO CH 4 F λ [erg/s/cm 2 /µm] 1e-13 1e-14 Na I H 2 O H 2 O H 2 O NH 3 1e-15 1e-16 V R I Z J H K L M 1e-17 1e-18 1 10 λ[µm]
Model grids for cool and ultracool dwarfs Allard et al. 1997 NextGen: molecular line blanketing, no condensation Casagrande et al. 2008 Golimowski et al. 2004 Vrba et al. 2004
Model grids for cool and ultracool dwarfs Allard et al. 1997 Allard et al. 2001 Freytag et al. 2010 Allard et al. in prep. 8 Years a,er: updated opacities, line profiles, abundances, and a new cloud model! Casagrande et al. 2008 Golimowski et al. 2004 Vrba et al. 2004
Model Atmospheres: Limb Darkening Relative Flux 1.00 0.95 0.90 0.85 0.80 0.75 0.70 0.2 0.4 0.6 0.8 1.0 µ Limb darkening curves of a 3500K M dwarf for IRAC 3.6, 4.5, 8.0 μm bands (blue, green, red): solid ATLAS models dashed PHOENIX fully molecular line blanketed models dotted free fit The shaded area is not passed in transit, thus unconstrained by lightcurve fitting Knutson et al. 2011
Extrasolar planets Transmission spectroscopy 1.000 UT 2007 Jun 29, 8.0 µm UT 2008 Jul 14, 8.0 µm UT 2009 Jan 9, 3.6 µm UT 2009 Jan 17, 4.5 µm Relative Flux 0.998 0.996 0.994 Relative Flux 0.992 0.0005 0.0000-0.0005-0.0010 1.000 UT 2009 Jan 25, 8.0 µm UT 2009 Jan 28, 3.6 µm UT 2009 Jan 30, 4.5 µm UT 2009 Feb 2, 8.0 µm Relative Flux Relative Flux 0.998 0.996 0.994 0.992 0.0005 0.0000-0.0005-0.0010-0.10-0.05 0.00 0.05-0.10-0.05 0.00 0.05-0.10-0.05 0.00 0.05-0.10-0.05 0.00 0.05 Time from Predicted Transit Center [d] Multi-wavelength IRAC transit observations of Gl 436b (Knutson et al. 2011)
Limb Darkening and Transmission Spectroscopy CH4 CH4 measured transit depths w/ ATLAS limb darkening (red circles) CO2 CO PHOENIX limb darkening zero limb darkening blue, green: CH4, COdominated planetary atmosphere models Knutson et al. 2011
Next Generation of PHOENIX models MUSE/BT-Settl (Allard, Homeier & Freytag) & ACES-Cond (Husser, Hauschildt et al.) grids Super(giants) & main sequence down through brown dwarf into exoplanet regime Extensive coverage of metallicities and α-enhancements 1D static, but with spherical symmetry Close feedback with CO5BOLD RHD simulations Detailed limb darkening or intensity output Hvala for funding through the programme Astroinformatics: Application of IT in Astronomy and Close Fields (PI D. Jevremović) & for your attention!