Abundances of Refractory Elements for Planet-Host Stars
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Abundances of Abundances of Refractory Elements Refractory Elements for Planet-Host Stars for Planet-Host Stars Lee, Sang-Gak Seoul National University Kim, Kang-Min Korea Astronomy and Space Science Institute 2009. 10. 9. Kang, Wonseok Seoul National University
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Abundances of Refractory Elements for Planet-Host Stars. Lee, Sang-Gak Seoul National University Kim, Kang-Min Korea Astronomy and Space Science Institute. 2009. 10. 9. Kang, Wonseok Seoul National University. OUTLINE. OUTLINE. Introduction Observations Process Measure the EWs - PowerPoint PPT Presentation
Transcript of Abundances of Refractory Elements for Planet-Host Stars
Abundances ofAbundances ofRefractory Elements Refractory Elements for Planet-Host Starsfor Planet-Host Stars
Lee, Sang-GakSeoul National University
Kim, Kang-MinKorea Astronomy and Space Science Institute
2009. 10. 9.
Kang, WonseokSeoul National University
The 4The 4thth Workshop on Extra-solar Planet Search with Accurate Radial Velocity Workshop on Extra-solar Planet Search with Accurate Radial Velocity Measurements in Japan, 2009Measurements in Japan, 2009
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OUTLINEOUTLINEOUTLINEOUTLINEIntroductionObservationsProcess Measure the EWs Determine the parameters of model atmosphere The abundances analysis
Statistics Radial velocities Model parameters
AbundancesSummary
The 4The 4thth Workshop on Extra-solar Planet Search with Accurate Radial Velocity Workshop on Extra-solar Planet Search with Accurate Radial Velocity Measurements in Japan, 2009Measurements in Japan, 2009
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INTRODUCTIONINTRODUCTIONINTRODUCTIONINTRODUCTIONAbundances for Planet-Host Stars (PHSs) Information of protoplanetary circumstance
Dust and planetesimal fomation in protoplanetary disks Stellar atmosphere conserves the primordial composition
Criteria for the planet-searchingPossibility to find the relationship between stellar abundance and exoplanet properties
Abundances of Refractory Elements Important in condensation process in the early stage of protoplan
etary disksespecially near the host star, the inside of ice line
Earth-life lives on the surface which is relatively abundant in refractory elements
Metabolism
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OBSERVATIONSOBSERVATIONSOBSERVATIONSOBSERVATIONSObservation In 2008 and 2009 With BOES at BOAO (Bohyunsan Optical Astronomy Observatory) Obtain the spectra of 98 star samples
Selected by the magnitude and declination.64 Known PHSs 34 Unknown samples
R ~ 30,000 / 45,000 (fiber: 300μm / 200μm) S/N ~ 100-300 at 5500Å
Samples for This Work Limited to G-type stars – 52 stars
Known PHSs – 34 / Unknown - 18
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SAMPLESSAMPLESSAMPLESSAMPLES
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PROCESSPROCESSPROCESSPROCESSMeasurement of EWs Using TAME program ( SSPEC at previous workshop)
Tools for Automatic Measurement for Equivalent-widths Total 13555 EWs of 52 stars ( Fe : 6246 / Others : 7309 )
Fit with Gaussian / Voigt profileLine list ; Gilli et al. 2006 / Cohen et al. 2009 / VALD15 elements
Calculate RVs from the center wavelength of fitting profiles
Determination of Model Atmosphere Parameters Using MOOGFE code with MOOG code & Kurucz ATLAS9 model Self-consistent fine analysis for Fe I/II lines
Calculate abundance of iron lines with starting model atmosphereCheck the slopes of iron abundancesAdjust the parameters of model atmosphereRemake the model atmosphere with new parameters(Iterate these processes)
For the Sun [Fe/H] = 0.00, TEff = 5823, log g = 4.41, ξ t = 0.98
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STATISTICSSTATISTICSSTATISTICSSTATISTICSModel Parameters Compared with 3 References
Cayrel et al. 2001 SPOCS Catalog (Valenti & Fischer, 2005) Gilli et al. 2006
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STATISTICSSTATISTICSSTATISTICSSTATISTICSRV Results Calculated by TAME fitting results Compared with the references
SIMBADGeneral Catalogue of
Stellar Radial Velocities (1953, 1979)
The Geneva-Copenhagen Survey (2004)
SPOCS catalog Valenti & Fischer 2005
Difference average & σ ΔRV [km/s] = RVTHIS – RVSIMBAD
- for each star
NLines / σLines [km/s]
- the lines for each star
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STATISTICSSTATISTICSSTATISTICSSTATISTICSAbundance Difference (Gilli et al. 2006)
Hyperfine structure
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STATISTICSSTATISTICSSTATISTICSSTATISTICSAbundance Average & σ
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESMetallicity [Fe/H]
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESMg I (α element)
Background small points from Bensby et al. 2005 / Mishenina et al. 2004 / Soubiran et al. 2005
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESSc II (α element)
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESTi I (α element)
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESMn I (iron-peak element)
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESZn I (iron-peak element)
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ABUNDANCESABUNDANCESABUNDANCESABUNDANCESBa II
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SUMMARY & FURTURE WORKSSUMMARY & FURTURE WORKSSUMMARY & FUTURE WORKSSUMMARY & FUTURE WORKSWe examined the abundances of 15 elements for 52 G-type samples ( PHSs : 34 )
[Mn/Fe] is high for PHSs The more Mn & Zn lines have to be added The synthetic spectrum with hyperfine structure
[Sc/Fe] and [Ti/Fe] tend to increase for PHSs in [Fe/H] < 0 Need more samples in [Fe/H] < 0
[Ba/Fe] of single-planet system is higher than that of multi-planet system
We plan to estimate abundance of Carbon, Oxygen, Sulfur Sulfur metabolism in the early stage of life-evolution
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