High Resolution High Resolution Spectroscopy of Stars Spectroscopy of Stars with Planets with Planets Won-Seok Kang Seoul National University 2010. 10. 6. Sang-Gak Lee, Seoul National University Kang-Min Kim, Korea Astronomy and Space science Institu CHEMICAL ABUNDANCE OF PLANET-HOST STAR
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High Resolution Spectroscopy of Stars with Planets
High Resolution Spectroscopy of Stars with Planets. CHEMICAL ABUNDANCE OF PLANET-HOST STAR. Won-Seok Kang Seoul National University 2010. 10. 6. Sang-Gak Lee, Seoul National University Kang-Min Kim, Korea Astronomy and Space science Institute. INTRODUCTION. - PowerPoint PPT Presentation
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High Resolution High Resolution Spectroscopy of Stars Spectroscopy of Stars
with Planetswith Planets
Won-Seok Kang Seoul National University
2010. 10. 6.
Sang-Gak Lee, Seoul National UniversityKang-Min Kim, Korea Astronomy and Space science Institute
CHEMICAL ABUNDANCE OF PLANET-HOST STAR
INTRODUCTIONINTRODUCTION
• Why we study chemical abundances of host stars – Conserve primordial abundances of planetary systems
• Related with planet formation process
– Find the relation between abundances and planets by observations
• Describe planet formation process in more detail• Select proper candidates with interesting planets
– Super-Earths and habitable planets
• What we can to with GMT high-resolution spectroscopy – Perform abundance analysis for more faint star
• Transiting planet-host star, M dwarf
– Obtain abundances and stellar parameters of more late-type stars
• Avoid strong molecular bands and pressure-broadened atomic lines
2GMT Workshop 2010 at SNU
PLANET AND METALLICITYPLANET AND METALLICITY
• Fischer and Valenti (2005) I– Spectroscopic analysis of ~1000 stars– For selecting planet-host stars
• Stars with planets were selected with period < 4 years and K > 30 m/s (gas giant planets)
• Stars without planets have been verified by observations of over 10 times for 4 or more years
– Calculate the planet-host ratio for each [Fe/H] bin
• Planet-host ratios are exponentially increasing with increasing metallicity
3GMT Workshop 2010 at SNU
Fischer and Valenti 2005
[Fe/H]0.21003.0)( planetP
PLANET AND METALLICITYPLANET AND METALLICITY
• Fischer and Valenti (2005) II– Suggest the relation between maximum of total planet mass
and metallicity• Total planet mass is related with protoplanetary disk mass ⇒ upper limit of total planet mass is increasing with increasing
[Fe/H]
• Planet mass from radial velocity measurement is MJ sini, which
means that this planet mass is lower limit of exact value
• So, need to know exact planet mass
4GMT Workshop 2010 at SNUFischer and Valenti 2005
METHOD OF ABUNDANCE METHOD OF ABUNDANCE ANALYSISANALYSIS
• Observations (166 FGK-type stars)– BOES at BOAO 1.8m telescope – R ~ 30,000 or 45,000 / SNR ~ 150 at 5500Å– Planet-host stars : 93 (74 dwarfs)– Comparisons : 73 (70 dwarfs) ← stars without known planets
• Abundance analysis – Kurucz ATLAS9 model grids and MOOG code – Measure EWs of Fe lines (TAME developed by IDL)– Determine model parameters by fine analysis (MOOGFE)
• Iteratively run MOOG code and ATLAS9
– Estimate abundances of 13 elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, S)
• Measuring EWs of elemental lines (TAME)• Comparing observational spectrum with synthetic spectrum
–
5GMT Workshop 2010 at SNU
METHOD OF ABUNDANCE METHOD OF ABUNDANCE ANALYSISANALYSIS
• TAME and MOOGFE
6GMT Workshop 2010 at SNU
Tools for Automatic Measurement of Equivalent-widths
Result of MOOGFE for the Sun
Excitation potential
Equivalent-width
Fe I Fe II
Model parameterslog eps(Fe) = 7.53 dex Teff = 5765 K
log g = 4.46 dex ξt = 0.82 km/s
Automatically find model parameters by iterations
By estimating the trend of iron abundance for excitation potential or equivalent width, and the abundance difference between Fe I and Fe II
METALLICITY HISTOGRAMMETALLICITY HISTOGRAM
• Metallicity distribution – Mean value of PHS is 0.13
dex higher than that of comparison
– Planet-Host Stars are more concentrated at higher [Fe/H]
• Comparisons are more widely distributed overall
• In low-metallicity, comparisons are more than PHSs
• In high-metallicity, PHSs are much more than comparisons
7GMT Workshop 2010 at SNU
<[Fe/H>-0.06
<[Fe/H]> +0.07
Only dwarfs
74 PHSs70 Comparions
METALLICITY AND PLANET METALLICITY AND PLANET PROPERTIESPROPERTIES
• [Fe/H] and Planet mass, MJsini– Increase with increasing [Fe/H]
• Similar result to Fischer and Valenti (2005)
– HD 114762• Known as spectroscopic binary• Companion is M6 dwarf at the
distance of 130 AU • Exceptional case or new evidence?
– For verifying, more samples in the range of low-metallicity will be required
8GMT Workshop 2010 at SNU
In the case of multiple-planetary system, total planet mass is indicated
These planetary masses represent MJsini , which is less than MJ
HD 114762 b
Only dwarfs
[Fe/H] vs. Planet Mass
Only 4 samples
METALLICITY AND PLANET METALLICITY AND PLANET PROPERTIESPROPERTIES
9GMT Workshop 2010 at SNU
Only dwarfs
• Metallicities and Planet properties– Hot jupiters are concentrated in
the region of [Fe/H] > 0 • It can support the relation
between migration and metallicity (Livio & Pringle, 2003)
• A Few stars in low-metallicity region
– In the region of low-metallicity, about half of host stars have relatively low-mass multiple planets.
• 2 of 5 planet-host stars have low-mass multiple planets
X : semi-major axisY : [Fe/H] Size of circle : planet mass
HD 114762 b
ABUNDANCE RESULTSABUNDANCE RESULTS
• [X/Fe] vs. [Fe/H] – Averaged for each [Fe/H]
bin– For most elements,
statistical difference between two groups ~ 0.03 dex
• [Mn/Fe] ratio– Difference between two
groups ~ 0.10 dex– Hyperfine structure
• It is necessary to confirm this difference by synthetic spectra and high S/N observational spectra
10GMT Workshop 2010 at SNU
Chemical Abundance Trend ; [Fe/H] vs. [X/Fe]
Only dwarfs
Red : Planet-Host StarsBlue : Comparisons
• Bin size : 0.2 dex• Center of each [Fe/H] bin : -0.5, -0.3, -0.1, +0.1, +0.3, +0.5
ABUNDANCE RESULTSABUNDANCE RESULTS
11GMT Workshop 2010 at SNU
HD 114762 b
[Mn/H] vs. planet mass• [Mn/H] and Planet mass– Maximum of planet mass are
increasing in low [Mn/H] range and decreasing in high [Mn/H] range
– Turn-off point of trend is located at solar Mn abundance
– It seems that the high [Mn/H] ratio has suppressed the massive planet formation
DIFFICULTIESDIFFICULTIES
12GMT Workshop 2010 at SNU
• Most of planets were detected by radial velocity method – Don’t know exact mass of planet– Samples are limited to almost nearby stars– Solution ; transiting planet
• Transit observation gives us more accurate mass of planet• Transit observation is available for faint and distant stars
• Lack of low-metallicity star– More low-metallicity stars are required to verify the relation between
planet properties and abundances– It seems to be easier to find Neptune-mass planets in low-metallicity
stars (Sousa et al. 2009)• They have only three Neptune-mass samples • Expect that more low-metallicity stars will be detected, in the near future
PRELIMINARY TESTPRELIMINARY TEST
13GMT Workshop 2010 at SNU
JM
iM J sin
Transiting planets
Radial velocity method
• Homogeneous studies of 30 transiting extrasolar planets (Southworth, 2010)– Provide the properties of planets and host
stars
• Test the relation for only transiting planets – Maximum of planet mass is decreasing with
increasing [Fe/H] – Inverse trend for the previous result of
samples detected by radial velocity method – Problems
• No stars of metallicity less than -0.2 dex • It seems that there are two groups of planet mass• Metallicities were adopted from several references
– Solutions • More low-metallicity stars with transiting planets• Perform abundance analysis in uniform method and
with the same instrument
WHAT WE CAN DO WITH GMTWHAT WE CAN DO WITH GMT
• Detailed abundances of host stars with transiting planets– Potential to detect new transiting planets in the near future
• HATNet, Kepler, CoRoT, SuperWASP, SWEEPS
– There are already 37 planets detected by transit in this year– Host stars are relatively faint, V ~ 10-15– Magnitude limit of transit observations will be fainter ⇒ GMT
14GMT Workshop 2010 at SNUhttp://exoplanet.eu
Number of planets by year of discovery
2010 (37)2009 (10) 2008 (17)2007 (19)
WHAT WE CAN DO WITH GMTWHAT WE CAN DO WITH GMT
• Abundances of M dwarfs using GMTNIRS– Advantages
1. Easy to detect new exoplanets or extraterrestrial lives– Host star is less massive (radial velocity method)
» Less massive exoplanets (super-earths)– Habitable zone is closer to host star (extraterrestrial life)
» Short period and probability of transits
2. Life time in the stage of main-sequence – Enough time for life evolution
3. The large number of M dwarfs in the Galaxy
– Disadvantages 1. Faint at visible wavelength ⇒ large telescope, GMTNIRS2. Strongly pressure-broadened atomic lines, and strong
molecular bands in visual wavelength range ⇒ GMTNIRS