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 Corr-Coef -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 Corr-Coef of [X/H] 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