Stars with and without planets: Where do they come from? Vardan Adibekyan (CAUP/IA) With the contribution of: J. Gonz´alezHern´andez,E. Delgado Mena, S. Sousa, N. Santos, P. Figueira, G. Israelian The Milky Way Unravelled by Gaia 2 December, 2014, Barcelona, Spain Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Introduction to Condensation Temperature When the temperature in the stellar disks drops (with time or with distance from the star), the heaviest com- pounds (first) began to form solid/liquid droplets, a process called condensation. The condensation temperature (Tc) for different ele- ments is different and relates with the mass of the par- ticles that become solid. Low Tc elements - volatiles High Tc elements - refractories (easily form dust) Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion [X/Fe] vs. Tc Figure: Melend´ezet al. (2009). Anomalous volatile-to-refractory ratio of the Sun when compared to solar twins. Refractories remained in rocky planets (Ramirez et al. 2009,2010). Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion [X/Fe] vs. Tc 0.15 0.10 0.1 O Eu Nd Y 0.10 C S Cu Eu Sr Nd Zr C Zn NaCu Zr Single: 32 stars O Na Mn Mg VCe Y SiMg BaVSr SUN-STARS 0.05 CrSiCoNi BaCaTi Sc S Mn CrNi CeCa AlSc + 0.00 Zn Al 0.0∆ [X/Fe] SUN-STARS Co Ti |S/N| = 831 − 371 -0.05 -0.10 -0.1 0.05 C S [X/Fe] Zn ∆ -0.15 HD 93385 ([Fe/H]=+0.02, mp= 8.4 MEARTH, NP = 2) HD 134060 ([Fe/H]=+0.14, mp=11.2 MEARTH, NP = 2) 0 500 T (K)C 1000 1500 0 500 T (K)C 1000 1500 Na Mg Sc Zn Cu CoEuNi VSr 0.15 O Cu Eu Zn Al 0.1 O Mn Si BaCa Ti Zr Al Sr Y Cr Ce Nd 0.10 C Na Co V Sc Zr Mn Ni Ti Ba Zr SUN-STARS Mn Y 0.05 S CrSiMg SrCa Nd O NaCu CrNi Ca 0.0∆ [X/Fe] SUN-STARS Sc Ce S SiMgCo V TiAl 0.00 0.00 Ba C Ce Nd -0.05 Y -0.10 -0.1 Eu [X/Fe] ∆ -0.15 HD 45184 ([Fe/H]=+0.05, mp=12.7 MEARTH, NP = 1) HD 189567 ([Fe/H]=-0.24, mp=10.0 MEARTH, NP = 1) 0 500 T (K)C 1000 1500 0 500 T (K)C 1000 Eu 1500 TEFF-TSUN=225K Logg-LoggSUN = 0.30 O Zr 0.15 Ce C Sr Zr -0.05 Zn Eu BaSr Nd 0.1 0.10 S Ca Y S BaVCe Y SUN-STARS S/N>250 -0.30 < [Fe/H] < 0.50 Cu Mg Zn Cu Mn CrMgCo TiAl SUN-STARS Si Ca 0.05 C Na CrCoNi V TiAl Na SiNi NdSc Sc 0.0∆ [X/Fe] SUN-STARS 0.00 Mn O Ba Al -0.05 -0.10 -0.1 [X/Fe] -0.10 S ∆ Zn -0.15 HD 1461 ([Fe/H]=+0.20, mp= 5.9 MEARTH, NP = 2) HD 96700 ([Fe/H]=-0.18, mp= 9.0 MEARTH, NP = 2) 0 500 T (K)C 1000 1500 0 500 T (K)C 1000 1500 [X/Fe] O C Na ∆ Cu Ni 0.15 Sr CrCo SZn Nd 0.1 Zn Mn Si V Sc 0.10 O MgEu Zr Mn BaCa Sc Y Mg Y Cu VSr AlSc O Eu Ce SUN-STARS Ti CeCa 0.05 C Mn CrSiNi BaCeCa Y Cu CrNi Ti Zr Ti Na Co 0.0∆ [X/Fe] SUN-STARS SiMg V 0.00 C Na Co NdAl -0.15 Sr -0.05 S -0.10 -0.1 Eu Nd Zr [X/Fe] Ba ∆ -0.15 HD 31527 ([Fe/H]=-0.17, mp=11.5 MEARTH, NP = 3) HD 134606 ([Fe/H]=+0.27, mp= 9.3 MEARTH, NP = 3) 0 500 T (K)C 1000 1500 0 500 T (K)C 1000 1500 Nd Sr 0.15 MgEu Sr Na Planet-host: 29 stars 0.1 Zn Ce Al Zr Nd Y Zr -0.20 0.10 O Cu V O Eu CeCa Ba Ti Sc Cu Mn Ni V + SUN-STARS 0.05 Mn CrCoNi Ca SZn CrSiCo TiAlSc |S/N| = 872 − 438 C Na Si Y 0.0∆ [X/Fe] SUN-STARS C Mg 0.00 S -0.05 -0.10 -0.1 -0.25 [X/Fe] ∆ -0.15 HD 10180 ([Fe/H]=+0.08, mp=11.8 MEARTH, NP > 3) HD 160691 ([Fe/H]=+0.30, mp=10.6 MEARTH, NP > 3) 0 500 1000 1500 0 500 1000 1500 0 500 1000 1500 TC (K) TC (K) TC (K) Figure: Gonz´alezHern´andezet al. (2013). No (significant) peculiar abundance ratio No evidence of relation between volatile-to-refractory abundance ratio and presence of rocky planets (Gonz´alezHern´andezet al. 2010,2013). Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Contradictory results { why? What is/are the main factor(s) responsible for the trends with Tc? Does terrestrial planet formation leave chemical imprints in the atmospheres of their host stars? The data is from Gonz´alezHern´andez et al. (2010,2013) The ages are from GCS - Casagrande et al. (2011) Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and stellar age Solar analogs Solar twins Figure: Adibekyan et al. (2014). Tc slope strongly correlates with the stellar age Older stars show lower refractory-to-volatile ratio independently of the presence of planets Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and Galactic Chemical Evolution For FGK dwarfs chemical abundances is not a function of age The Tc slope and age correlation is probably a reflection of the chemical evolution in the Galaxy What else relates to Galactic chemical evolution? The birth place:Rmean { mean of the apo- and pericentric distances. Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and Rmean Solar analogs Solar twins Figure: Adibekyan et al. (2014). Tc slope correlates with Rmean Stars with smaller Rmean show larger Tc slopes. Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and Rmean: Galactic abundance gradients Tc slope correlates with galactocentric distance? What do the other samples (data) say? Vardan Adibekyan Where do planet host stars come from? Very good (qualitative) agreement! Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and Rmean: Galactic abundance gradients [X/Fe] vs. TC using the Galactic abundance gradients of Galactic Cepheids from Lemasle et al. (2008, 2013). Figure: Lemasle et al. (2008, 2013). Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and Rmean: Galactic abundance gradients [X/Fe] vs. TC using the Galactic abundance gradients of Galactic Cepheids from Lemasle et al. (2008, 2013). Very good (qualitative) agreement! Figure: Lemasle et al. (2008, 2013). Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and planets Tc slope depends on stellar age and galactic birth place. What about the planets? Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope and planets Figure: Adibekyan et al. (2014). Solar analogues with planets show larger Tc slopes (PKS = 0.21). Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope, ages, and planets Figure: Adibekyan et al. (2014). Solar analogues with planets have older age (PKS = 0.20). Should be a detection bias. Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Tc slope, Rmean, and planets Figure: Adibekyan et al. (2014). Solar analogues with planets show smaller Rmean (PKS = 0.007). Chemical composition (e.g. Adibekyan et al. 2014) or F(r) (Haywood 2009) ? Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Planet hosts and Galactic disks Figure: Left - Haywood 2009. Right - Adibekyan et al. 2012. Metal-poor giant planet hosts mostly belong to the Thick disk (Haywood 2009) Metal-poor giant and small planet hosts mostly belong to the Thick disk (Adibekyan et al. 2012) Vardan Adibekyan Where do planet host stars come from? Introduction to Tc Tc slope: Previous works Tc slope: Galactic evolution Tc slope: Planets Conclusion Conclusion and open questions The age and Galactic birth place are determinant to establish the chemical properties of each star Solar analogues with planets mostly come from the inner Galaxy Metal-poor planet hosts come from the Galactic Thick disk Chemical conditions in the inner disk and thick disk are more favorable for planet formation (?) Need to be further explored ..