A complete CHARActerization of the HD189733 and the HD209458 systems Tabetha Boyajian Kaspar von Braun, Gregory A. Feiden, Daniel Huber, Sarbani Basu, Pierre Demarque, Debra A. Fischer, Gail Schaefer, Andrew W. Mann, Timothy R. White, Vicente Maestro, John Brewer, C. Brooke Lamell, Federico Spada, Mercedes Lopez-Morales, Michael Ireland, Chris Farrington, Gerard T. van Belle, Stephen R. Kane, Jeremy Jones, Theo A. ten Brummelaar, David R. Ciardi, Harold A. McAlister, Stephen Ridgway, P. J. Goldfinger, Nils H. Turner, Laszlo Sturmann
Full article: Boyajian et al. 2015, MNRAS, 447, 846 #111
The hot (super-sized) Jupiters HD189733b and HD209458b HD 189733 (K2 V) HD 209458 (G0 V)
Planet radii The radius anomaly Time Depth = (Rpl/R*)2 Host star radius must be known! Radius (RJ) Brightness 1.6 1.4 1.2 1.0 0.8 0.01 0.1 1 Mass (MJ) 10
Using the planet to learn about the star (special cases) The planet s RVs are observed for the transiting systems HD 189733 and HD 209458 à measured masses 300 150 50 km/s Snellen et al. (2010)
Classic @ CHARA Baines et al. (2007) Flux 0.6 σθ = 6.7% σθ = 1.5% 0.4 0.2 0 6 1.5 1.0 HD 189733 0.5 3 0 3 1 4 Wavelength (um) 3 4 1 Spectrum Photometry Synthetic Photometry 3 2 1 2 Wavelength (µm) σθ = 3.2% 2 Flux (10 12 Visibility2 0.6 2.0 rad-1) 1.0 0.8 2.5 s Å ) Spatial frequency (x108 0.4 Residual ( ) 0 0.8 Spectrum Photometry Synthetic Photometry 3.0 Fluxerg cm Visibility2 1.0 Spectrophotometry: Visible: SNIFS (.32 -.97um; R~1000) IR: uspex (0.7 2.5 um; R~400) 12 2 1 1 Residual ( ) Flux (10 erg cm s Å ) Interferometry: PAVO @ CHARA Baselines > 300m 0.2 0 1 HD 209458 3 0 3 1 Spatial frequency (x108 rad-1) 2 Wavelength (µm) Wavelength (um) 3 4
Model independent properties for both star and planet
Stellar mass and radius: Observations versus model predictions The radius discrepancy in eclipsing binaries à Evolutionary models have a hard time reproducing the radius of a star at a given mass. Figure from Carter et al. (2012)
Stellar mass and radius: HD189733 HD 189733 The radius discrepancy in eclipsing binaries à Evolutionary models are in excellent agreement with measured Mass and Radius for HD 189733 Figure from Carter et al. (2012)
Stellar Teff and radius: Observations versus model predictions Radius (R ) HD189733? Evolutionary models predict radii too small and Teffs too large compared to observations Boyajian et al. (2012) Teff (K)
Radius (R ) Stellar Teff and radius: HD189733 à Evolutionary models are NOT in excellent agreement with measured Teff and Radius for HD 189733 Boyajian et al. (2012) Teff (K)
WHY? HD 189733 mass and radius are in agreement, but not the Teff and radius à the luminosity is off by 35%!
Henry & Winn (2008) AGE COMPOSITION Metallicity CONVECTION Magneto-convection Star spots Reduced mixing length Radius (R ) α-element enhancement Helium abundance Solar mixture Prot ~ 11 days Premain sequence main sequence HD 189733 Teff (K)
Example: [Fe/H] = - 0.03 +/- 0.08 (Bouchy et al. 2005; Torres et al. 2008) AGE CONVECTION Magneto-convection Star spots Reduced mixing length Radius (R ) α-element enhancement Helium abundance Solar mixture main sequence Mixture: Teff (K) COMPOSITION Metallicity Preà Models require [M/H] = + 0.2 (@ 10 Gyr) 10 100 1000 Age (Myr) 1e4 Figure courtesy o
< Bf > ~ 40 100 G (Moutou et al. 2007; Pillitteri et al. 2014) AGE α-element enhancement Helium abundance Solar mixture <Bf>=1.5 kg <Bf>=2.5 kg Radius (R ) COMPOSITION Metallicity Models require ~1.5kG CONVECTION Magneto-convection Star spots Reduced mixing length Teff (K) DMEstar: Feiden & Chaboyer (2012, 2013), as described in Muirhead et al. (2014) and Malo et al. (2014)
AGE COMPOSITION Metallicity α-element enhancement Helium abundance Solar mixture CONVECTION Magneto-convection Star spots Reduced mixing length Fares et al. (2010); Llama et al. (2013)
Log g AGE COMPOSITION Metallicity Bonaca et al. (2012) partial residual CONVECTION Magneto-convection Star spots Reduced mixing length partial residual α-element enhancement Teff Helium abundance Solar mixture 3.7 Log Teff
Radius (R ) Radius (R ) A physically correct model solution Teff (K) Teff (K) YREC: MC modeling with mixing length and Helium set free (Helium limited to primordial)
Thank you.