A complete CHARActerization of the HD and the HD systems

Transcription

1 A complete CHARActerization of the HD and the HD 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

2 Full article: Boyajian et al. 2015, MNRAS, 447, 846 #111

3 The hot (super-sized) Jupiters HD189733b and HD209458b HD (K2 V) HD (G0 V)

4 Planet radii The radius anomaly Time Depth = (Rpl/R*)2 Host star radius must be known! Radius (RJ) Brightness Mass (MJ) 10

5 Using the planet to learn about the star (special cases) The planet s RVs are observed for the transiting systems HD and HD à measured masses km/s Snellen et al. (2010)

6 CHARA Baines et al. (2007) Flux 0.6 σθ = 6.7% σθ = 1.5% HD Wavelength (um) Spectrum Photometry Synthetic Photometry Wavelength (µm) σθ = 3.2% 2 Flux (10 12 Visibility rad-1) s Å ) Spatial frequency (x Residual ( ) Spectrum Photometry Synthetic Photometry 3.0 Fluxerg cm Visibility2 1.0 Spectrophotometry: Visible: SNIFS ( um; R~1000) IR: uspex ( um; R~400) Residual ( ) Flux (10 erg cm s Å ) Interferometry: CHARA Baselines > 300m HD Spatial frequency (x108 rad-1) 2 Wavelength (µm) Wavelength (um) 3 4

7 Model independent properties for both star and planet

8 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)

9 Stellar mass and radius: HD HD The radius discrepancy in eclipsing binaries à Evolutionary models are in excellent agreement with measured Mass and Radius for HD Figure from Carter et al. (2012)

10 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)

11 Radius (R ) Stellar Teff and radius: HD à Evolutionary models are NOT in excellent agreement with measured Teff and Radius for HD Boyajian et al. (2012) Teff (K)

12 WHY? HD mass and radius are in agreement, but not the Teff and radius à the luminosity is off by 35%!

13 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 Teff (K)

14 Example: [Fe/H] = / (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] = (@ 10 Gyr) Age (Myr) 1e4 Figure courtesy o

15 < Bf > ~ 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)

16 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)

17 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

18 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)

19 Thank you.