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Chemical Abundance Study of Planetary Hosting Stars P CHEMICAL ABUNDANCE STUDY OF PLANETARY HOSTING STARS P. Rittipruk and Y. W. Kang Department of Astronomy and Space Science Sejong University, Korea Planetary Hosting Stars Metallicity ∝ Probability of Hosting Planets Planetary Hosting Stars Planetary Hosting Stars 0.8 0.6 with planet 0.4 without planet 0.2 0.0 -0.2 -0.4 -0.6 Corr-Coef of [X/H] vs EP -0.8 -1.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 [M/H] Chemical abundances of 1111 FGK stars (Adibekyan et al, 2012) 1.2 c 0.8 0.4 0.0 -0.4 -0.8 Corr-Coef of [X/H] vs T with planet without planet -1.2 -1.5 -1.0 -0.5 0.0 0.5 1.0 [M/H] Chemical abundances of 1111 FGK stars (Adibekyan et al, 2012) HD 20794 ‘s Planets Earth to Sun = 1 AU Mass = 0.70 Msun Radius = 0.92 Rsun Distance = 6.06 pc Age = 14±6 Gyr (Bernkopf+2012) = 5.76±0.66 (Gyr)(Pepe+ 2011) bcde M sin i 0.0085 0.0076 0.0105 0.0150 (MJ) (2.7) (2.4) (4.8) (4.7) a(AU) 0.1207 0.2036 0.3499 0.509 P(days) 18.315 40.114 90.309 147.2 HD 47536 ‘s Planets ■ Mass = 0.94 Msun Earth to Sun = 1AU ■ Radius = 23.47 Rsun ■ Distance = 121.36 pc ■ Age = 9.33 Gyr (Silva+2006) HD 47536b HD 47536c** M sin i (MJ) 4.96 6.98 a(AU) 1.61 3.72 P(days) 430 2500 Observation CHIRON Echelle Spectrometer Wavelength cover : 4200 – 8800 A Narrow Slit (R = 120,000) SMART-1.5m at CTIO, La Serena, Chile Observed Spectrum Echelle Spectrum of HD20794 obtained using CHIRON Spectrometers Reduced Spectrum Spectrum of HD20794 after reduction plotted with synthesis spectrum Algorithms Rotational Velocity (v sin i) Determination Reiners & Schmitt (2003) ⁄ sin 0.610 0.062 0.027 0.012 0.004 1.117 0.048 0.029 0.024 0.012 Continuum level Equivalent Width (EW) Using URAN: (Gaussian Profile fitting) EW - Fe I 127 lines - Fe II 30 lines Stellar Parameters ■ Surface Temperature (Teff) ■ Microturbulent velocity (ξt) • Excitation Equilibrium ■ Surface Gravity (Log g) • Equivalent width ■ Metallicity ([Fe/H]) independence • Ionization equilibrium ■ Rotational Velocity (v sin i) Model Atmosphere Grid Kurucz & Castelli (2005): new ODFs with no convective overshooting Iron (Fe) Abundance Teff = 5510 K, log g = 4.41, ξ = 0.91, [Fe/H] = -0.42 Ionization Balance => log g HD20794’s Results The selected model parameters are: Effective temperature: Teff = 5510 K Surface gravity: log g = 4.8 Micro-turbulent velocity: Vmicro = 0.91 km/s projected velocity: V sin i = 2.64 km/s The abundances of iron are: ■ log N ( Fe I ) = 7.076 ± 0.031 ( 101 lines) ■ log N ( FeII ) = 7.066 ± 0.013 ( 23 lines ) ■ The solar abundance of iron is log N (Fe) = 7.50 – [Fe I /H] = -0.424 – [Fe II /H] = -0.434 HD20794’s Parameters Fe I Fe II Spectroscopic parameters: Teff = 4400 K, log g = 1.80, ξt = 1.5 km/s Signature of Planet Formation [Fe/H]=-0.42 Signature of Planet Formation Spectroscopicin HD parameters:47536 ? Teff =0.6 4400 K, log g = 1.80, ξt = 1.5 km/s 0.4 [Fe/H]=-0.54 Gd 0.2 Eu SmNd Th 0.0 Dy RuMo Er O Pr Al Rb Mg C La W -0.2 VBa Na Co Zr Zn Si log N Sr Ti K Nb Sc -0.4 Ti Zr Y FeNi CeCa Cu Cr -0.6 Mn -0.8 -1.0 0 500 1000 1500 2000 TC (K) Signature of Planet Formation 1.0 Ru (He 24.6 eV) 0.5 PbW O Pr Al DyCa TiMgMo C 0.0 Si NdThSc Mn Na SrEu Zn Cr Ni La Zr Fe Ce Y Rb -0.5 Sm Ag log N Gd Co -1.0 Ba -1.5 (H 13.6 eV) -2.0 0 1020304050 2nd (eV) Sign of accretion in HD 47536? 0.6 H 13.6 eV 0.4 He 24.6 eV 0.2 0.0 -0.2 log N -0.4 -0.6 -0.8 -1.0 10 15 20 25 30 35 2nd (eV) Accretion ??? H Ca star Interstellar Medium deficiency of Calcium and other elements with second ionization potential close to 13.6 eV Solar R-process HD 20794 Solar R-process HD 47536 2 Cu I HD 47536 1 Sr I Rb IZr II Zr I Ba II Ba I Y II Mo I 0 Y I Ru I log N Nd II Gd II Nb I Ce II Dy II Sm II La II Er II -1 W I Pr II Eu II Th II -2 40 60 80 100 Z Galactic Chemical Evolution? Spina et al. 2016 Summary & Future work The abundance of 35 elements and its pattern of planetary host star HD 20794 & HD 47536 were investigated. – HD 20794 has no correlation between abundance vs. Tc (K) and abundance vs. 2nd ionization potential. – Deficiency of Cobalt (Co), Barium (Ba), and Gadolinium (Gd) The p-process element (Ni) and r-process element (Eu) show slightly overabundance. while we found under abundance of s- process abundance (Ba). It would be interesting to compare our result of HD20794 with result other metal-poor planetary hosting star. Summary & Future work The HD 47536 star is a halo giant with relative overabundances of heavy elements, produced by previous stellar generations ■ The atmosphere of HD 47536 might be influenced by: 1) the accretion of dust-gas mixture from circumstellar envelope. 2) the accretion of hydrogen and helium from interstellar medium. Summary & Future work We found correlation between metallicity and the abundance dependency with 2nd ionization potential and Condensation temperature. The stars with and without planet show same correlation between dependency coefficient and metallicity. Summary & Future work Name RA Dec V Sp Type Temp Fe/H Log g Vsin i Rot P HD 27442 04 16 29 -59 18 07 4.44 K2 IV a 4749 0.22 3.3 2.9 115.11 HD 27631 04 19 45 -41 57 37 8.25 G3IV - HD 28185 04 26 26 -10 33 02 7.81 G5 5482 0.24 - HD 290327 05 23 22 -02 16 39 8.96 G8V 5552 -0.11 - HD 30562 04 48 36 -05 40 27 5.77 F8V 5861 0.24 4.08 17.3 4.79 HD 30856 04 50 18 -24 22 08 8.07 K0III 4982 -0.06 3.4 HD 31527 04 55 38 -23 14 31 7.48 G0V 1.1 0 HD 33142 05 07 36 -13 59 11 8.13 K0III 5052 0.05 - HD 33283 05 08 01 -26 47 50 8.05 G3V 5995 0.37 3.2 18.97 HD 38529 05 46 34 +01 10 05 5.94 G4 IV 5697 0.27 3.9 31.64 HD 38801 05 47 59 -08 19 40 8.26 K0IV 5222 0.26 - HD 38858 05 48 35 -04 05 41 5.97 G4V 4.2 HD 39194 05 44 32 -70 08 37 8.08 K0V 5205 -0.61 4.53 - HD 40307 05 54 04 -60 01 24 7.17 K2.5V 4977 -0.31 4.47 1.6 HD 41004 A 05 59 49 -48 14 22 8.65 K1 V 5035 -0.09 - HD 44219 06 20 14 -10 43 30 7.69 G2V 5752 0.03 - HD 45184 06 24 44 -28 46 48 6.37 G1.5V - HD 45364 06 25 38 -31 28 51 8.08 K0V 5434 -0.17 4.38 1 km/s 32 day HD 45652 06 29 13 +10 56 02 8.1 G8-K0 5312 0.29 HD 46375 06 33 12 +05 27 46 7.94 K1 IV 5199 0.24 4.53 0.86 58.81 HD 47186 06 36 09 -27 37 20 7.8 G5V 5675 0.23 - HD 50499 06 52 02 -33 54 56 7.22 G IV 5902 0.23 4.21 16.58 HD 52265 07 00 18 -05 22 01 6.3 G0 V 6159 0.21 4.67 13.54 HD 60532 07 34 03 -22 17 46 4.45 F6IV-V 6095 -0.26 5.3 HD 69830 08 18 23 -12 37 55 5.95 K0V 5385 -0.05 4.5 10.06 HD 70573 08 22 50 +01 51 34 8.7 G1-1.5V 5737 -0.18 - HD 70642 08 21 28 -39 42 19 7.17 G5 IV-V 5670 0.16 0.3 141.62 HD 73267 08 36 18 -34 27 36 8.9 G5V 5317 0.03 - HD 75289 08 47 40 -41 44 12 6.35 G0 V 6120 0.29 4.14 15.27 HD 82943 09 34 50 -12 07 46 6.54 G0 5874 0.32 1.35 41.96 HD 85512 09 51 07 -43 30 10 7.67 K5V 4715 -0.33 4.1 HD 90156 10 23 55 -29 38 44 6.95 G5V 5599 -0.24 - NGC 24233 07 37 09 -13 54 24 9.45 0.14 - THANK YOU.
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