J/MNRAS/456/2636 Kepler-10 chemical composition (Liu+, 2016)
The detailed chemical composition of the terrestrial planet host Kepler-10.
Liu F., Yong D., Asplund M., Ramirez I., Melendez J., Gustafsson B.,
Howes L.M., Roederer I.U., Lambert D.L., Bensby T.
<Mon. Not. R. Astron. Soc., 456, 2636-2646 (2016)>
=2016MNRAS.456.2636L 2016MNRAS.456.2636L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Abundances
Keywords: planets and satellites: formation -
planets and satellites: terrestrial planets; stars: abundances -
stars: individual: Kepler-10
Abstract:
Chemical abundance studies of the Sun and solar twins have
demonstrated that the solar composition of refractory elements is
depleted when compared to volatile elements, which could be due to the
formation of terrestrial planets. In order to further examine this
scenario, we conducted a line-by-line differential chemical abundance
analysis of the terrestrial planet host Kepler-10 and 14 of its
stellar twins. Stellar parameters and elemental abundances of
Kepler-10 and its stellar twins were obtained with very high precision
using a strictly differential analysis of high quality
Canada-France-Hawaii Telescope, Hobby-Eberly Telescope and Magellan
spectra. When compared to the majority of thick disc twins, Kepler-10
shows a depletion in the refractory elements relative to the volatile
elements, which could be due to the formation of terrestrial planets
in the Kepler-10 system. The average abundance pattern corresponds to
∼13 Earth masses, while the two known planets in Kepler-10 system
have a combined ∼20 Earth masses. For two of the eight thick disc
twins, however, no depletion patterns are found. Although our results
demonstrate that several factors [e.g. planet signature, stellar age,
stellar birth location and Galactic chemical evolution (GCE)] could
lead to or affect abundance trends with condensation temperature, we
find that the trends give further support for the planetary signature
hypothesis.
Description:
We obtained high resolution and high SNR spectra with the
Canada-France-Hawaii Telescope (CFHT), the Hobby-Eberly
Telescope (HET) and the Magellan Clay Telescope.
We observed Kepler-10 with the Echelle SpectroPolarimetric Device for
the Observation of Stars at the CFHT during 2013 June. The spectral
revolving power is 68000 and the spectral range is 3800-8900Å.
We also observed Kepler-10 with the High Resolution Spectrograph (HRS)
on the HET at McDonald Observatory during 2011 May. A total
integration time of 6.8h was needed to achieve SNR>350 per pixel. The
spectrum has a spectral resolving power of 60000 and covers
4100-7800Å, with a gap of about 100Å around 6000Å.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 73 16 Stellar parameters of Kepler-10 and its
stellar twins
table2.dat 45 19 [X/H] for Kepler-10 and the average of
its thick disc stellar twins
tablea1.dat 25 251 Atomic line data adopted for the abundance
analysis
tablea2.dat 275 14 All the derived elemental abundances and
associated uncertainties of each programme star
with relative to Kepler-10
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Object Object name
11 A1 --- n_Object [bcd] Note on Object (1)
13- 16 I4 K Teff Effective temperature
18- 19 I2 K e_Teff rms uncertainty on Teff
21- 24 F4.2 [cm/s2] logg Surface gravity
26- 29 F4.2 [cm/s2] e_logg rms uncertainty on logg
31- 34 F4.2 km/s vturb Microturbulent velocity
36- 39 F4.2 km/s e_vturb rms uncertainty on vturb
41- 46 F6.3 [-] [Fe/H] Metallicity
48- 52 F5.3 [-] e_[Fe/H] rms uncertainty on [Fe/H]
54- 55 I2 % PThin Probability of thin disc (2)
57- 58 I2 % PThick Probability of thick disc (2)
60- 64 A5 --- Pop [thick/thin ] Population
65 A1 --- n_Pop [e] Note on Pop (1)
67- 69 F3.1 Gyr Age Age
71- 73 F3.1 Gyr e_Age rms uncertainty on Age
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Note (1): Notes as follows:
b = Parameters derived with HET data
c = Parameters derived with CFHT data
d = Parameters derived using Kepler-10 (HET) as the reference
e = HIP 101857 is assigned to the thin disc because of its abundance pattern
rather than kinematics
Note (2): Probabilities calculated based on kinematics (Ramirez et al., 2013
Cat. J/ApJ/764/78).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- El Element
8- 13 F6.3 [-] [X/H]Het Kepler-10 [X/H] derived with HET data,
relative to the Sun
15- 19 F5.3 [-] e_[X/H]Het rms uncertainty on [X/H]Het
21- 26 F6.3 [-] [X/H]CFHT Kepler-10 [X/H] derived with CFHT data,
relative to the Sun
28- 32 F5.3 [-] e_[X/H]CFHT rms uncertainty on [X/H]CFHT
34- 39 F6.3 [-] [X/H]tw Mean thick disc twins [X/H] derived
with respect to Kepler-10 (HET)
41- 45 F5.3 [-] e_[X/H]tw rms uncertainty on [X/H]tw
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm lambda Wavelength
10- 14 A5 --- El Element
16- 19 F4.2 eV EP Excitation potential
21- 25 F5.2 [-] loggf Oscillator strength
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Object Object name
12- 17 F6.3 [-] D[C/H] Average abundance difference [C/H] (HET-CFHT)
19- 23 F5.3 [-] e_D[C/H] Average abundance difference [C/H] (HET-CFHT)
26- 31 F6.3 [-] D[O/H] Average abundance difference [O/H] (HET-CFHT)
33- 37 F5.3 [-] e_D[O/H] Average abundance difference [O/H] (HET-CFHT)
40- 45 F6.3 [-] D[Na/H] Average abundance difference [Na/H] (HET-CFHT)
47- 51 F5.3 [-] e_D[Na/H] Average abundance difference [Na/H] (HET-CFHT)
54- 59 F6.3 [-] D[Mg/H] Average abundance difference [Mg/H] (HET-CFHT)
61- 65 F5.3 [-] e_D[Mg/H] Average abundance difference [Mg/H] (HET-CFHT)
68- 73 F6.3 [-] D[Al/H] Average abundance difference [Al/H] (HET-CFHT)
75- 79 F5.3 [-] e_D[Al/H] Average abundance difference [Al/H] (HET-CFHT)
82- 87 F6.3 [-] D[Si/H] Average abundance difference [Si/H] (HET-CFHT)
89- 93 F5.3 [-] e_D[Si/H] Average abundance difference [Si/H] (HET-CFHT)
96-101 F6.3 [-] D[S/H] Average abundance difference [S/H] (HET-CFHT)
103-107 F5.3 [-] e_D[S/H] Average abundance difference [S/H] (HET-CFHT)
110-115 F6.3 [-] D[Ca/H] Average abundance difference [Ca/H] (HET-CFHT)
117-121 F5.3 [-] e_D[Ca/H] Average abundance difference [Ca/H] (HET-CFHT)
124-129 F6.3 [-] D[Sc/H] Average abundance difference [Sc/H] (HET-CFHT)
131-135 F5.3 [-] e_D[Sc/H] Average abundance difference [Sc/H] (HET-CFHT)
138-143 F6.3 [-] D[TiI/H] Average abundance difference [TiI/H]
(HET-CFHT)
145-149 F5.3 [-] e_D[TiI/H] Average abundance difference [TiI/H]
(HET-CFHT)
152-157 F6.3 [-] D[TiII/H] Average abundance difference [TiII/H]
(HET-CFHT)
159-163 F5.3 [-] e_D[TiII/H] Average abundance difference [TiII/H]
(HET-CFHT)
166-171 F6.3 [-] D[V/H] Average abundance difference [V/H] (HET-CFHT)
173-177 F5.3 [-] e_D[V/H] Average abundance difference [V/H] (HET-CFHT)
180-185 F6.3 [-] D[Cr/H] Average abundance difference [Cr/H] (HET-CFHT)
187-191 F5.3 [-] e_D[Cr/H] Average abundance difference [Cr/H] (HET-CFHT)
194-199 F6.3 [-] D[Mn/H] Average abundance difference [Mn/H] (HET-CFHT)
201-205 F5.3 [-] e_D[Mn/H] Average abundance difference [Mn/H] (HET-CFHT)
208-213 F6.3 [-] D[Fe/H] Average abundance difference [Fe/H] (HET-CFHT)
215-219 F5.3 [-] e_D[Fe/H] Average abundance difference [Fe/H] (HET-CFHT)
222-227 F6.3 [-] D[Co/H] Average abundance difference [Co/H] (HET-CFHT)
229-233 F5.3 [-] e_D[Co/H] Average abundance difference [Co/H] (HET-CFHT)
236-241 F6.3 [-] D[Ni/H] Average abundance difference [Ni/H] (HET-CFHT)
243-247 F5.3 [-] e_D[Ni/H] Average abundance difference [Ni/H] (HET-CFHT)
250-255 F6.3 [-] D[Cu/H] Average abundance difference [Cu/H] (HET-CFHT)
257-261 F5.3 [-] e_D[Cu/H] Average abundance difference [Cu/H] (HET-CFHT)
264-269 F6.3 [-] D[Zn/H] Average abundance difference [Zn/H] (HET-CFHT)
271-275 F5.3 [-] e_D[Zn/H] Average abundance difference [Zn/H] (HET-CFHT)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Sep-2016