HIGH PRECISION ABUNDANCES OF THE OLD SOLAR TWIN HIP 102152: INSIGHTS ON Li DEPLETION FROM THE OLDEST SUN

Monroe, TalaWanda R.; Meléndez, Jorge; Ramírez, Iván; Yong, David; Bergemann, M.; Asplund, Martin; Bedell, Megan; Maia, M. Tucci; Bean, Jacob L.; Lind, Karin; Alves-Brito, Alan; Casagrande, Luca; Castro, M.; Nascimento, J.-D. do; Bazot, M.; Freitas, Fabrício C.

doi:10.1088/2041-8205/774/2/l32

Cited by 87 publications

(132 citation statements)

References 35 publications

(51 reference statements)

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“…This explains the low level obtained for the uncertainties of the stellar properties. Similar studies reported in the literature have claimed even lower (by a factor of 2) uncertainties, using this type of analysis for solar twins/analogues (Meléndez et al 2012;Monroe et al 2013). Morel et al (2013) provided an accurate determination of elemental abundances, which confirms that the chemical composition of HD 43587 is close to solar, except for a slight magnesium excess and an enhancement by one order of magnitude of lithium (+2.05 dex for HD 43587 versus +0.92 dex for the Sun).…”

Section: Spectroscopic Datasupporting

confidence: 85%

Seismic analysis of HD 43587Aa, a solar-like oscillator in a multiple system

Boumier

Benomar

Baudin

et al. 2014

A&A

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Context. The object HD 43587Aa is a G0V star observed during the 145-day LRa03 run of the COnvection, ROtation and planetary Transits space mission (CoRoT), for which complementary High Accuracy Radial velocity Planet Searcher (HARPS) spectra with S/N > 300 were also obtained. Its visual magnitude is 5.71, and its effective temperature is close to 5950 K. It has a known companion in a highly eccentric orbit and is also coupled with two more distant companions. Aims. We undertake a preliminary investigation of the internal structure of HD 43587Aa. Methods. We carried out a seismic analysis of the star, using maximum likelihood estimators and Markov chain Monte Carlo methods. Results. We established the first table of the eigenmode frequencies, widths, and heights for HD 43587Aa. The star appears to have a mass and a radius slightly larger than the Sun, and is slightly older (5.6 Gyr). Two scenarios are suggested for the geometry of the star: either its inclination angle is very low, or the rotation velocity of the star is very low. Conclusions. A more detailed study of the rotation and of the magnetic and chromospheric activity for this star is needed, and will be the subject of a further study. New high resolution spectrometric observations should be performed for at least several months in duration.

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Section: Spectroscopic Datasupporting

confidence: 85%

Seismic analysis of HD 43587Aa, a solar-like oscillator in a multiple system

Boumier

Benomar

Baudin

et al. 2014

A&A

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“…However, stars with low Na and Ni abundances in this paper cover a wide range of ages. Instead, HIP 102152 with [Na/Fe] = −0.044 and [Ni/Fe] = −0.026 (Monroe et al 2013) fits the Ni-Na relation shown in Fig. 12 almost exactly.…”

Section: [X/fe] -Tc Correlationsmentioning

confidence: 86%

“…As shown in Fig. 13 for the case of HD 20782 very different slopes are derived depending on whether one includes all elements or fit only elements with a condensation temperature T C > 900 K as in Ramírez et al (2009 Monroe et al (2013), who suggest that the low sodium (and nitrogen) abundance could be due to its high age (8 Gyr). However, stars with low Na and Ni abundances in this paper cover a wide range of ages.…”

Section: [X/fe] -Tc Correlationsmentioning

confidence: 99%

“…Recent precise determinations of abundances in four solar twin stars: HD 101364 (Meléndez et al 2012), HIP 102152 (HD 197027;Monroe et al 2013), 18 Sco (HD 146233; Meléndez et al 2014a), and HD 218544 show that the first three stars have a similar depletion of refractory elements as the Sun, whereas 18 Sco has a [X/Fe]-T C slope for elements from carbon to zinc similar to the majority of solar twin stars. Neutron capture elements in 18 Sco are, however, significantly more abundant than lighter elements with the same condensation temperature, and in HIP 102152 several elements (N, Na, Co, and Ni), have abundance ratios with respect to Fe that clearly fall below the [X/Fe]-T C trend for the other elements.…”

Section: Introductionmentioning

confidence: 99%

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High-precision abundances of elements in solar twin stars

Nissen

2015

A&A

242

302

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Context. High-precision determinations of abundances of elements in the atmospheres of the Sun and solar twin stars indicate that the Sun has an unusually low ratio between refractory and volatile elements. This has led to the suggestion that the relation between abundance ratios, [X/Fe], and elemental condensation temperature, T C , can be used as a signature of the existence of terrestrial planets around a star. Aims. HARPS spectra with S /N 600 for 21 solar twin stars in the solar neighborhood and the Sun (observed via reflected light from asteroids) are used to determine very precise (σ ∼ 0.01 dex) differential abundances of elements in order to see how well [X/Fe] is correlated with T C and other parameters such as stellar age. Methods. Abundances of C, O, Na, Mg, Al, Si, S, Ca, Ti, Cr, Fe, Ni, Zn, and Y are derived from equivalent widths of weak and medium-strong spectral lines using MARCS model atmospheres with parameters determined from the excitation and ionization balance of Fe lines. Non-LTE effects are considered and taken into account for some of the elements. In addition, precise (σ 0.8 Gyr) stellar ages are obtained by interpolating between Yonsei-Yale isochrones in the log g -T eff diagram. Results. It is confirmed that the ratio between refractory and volatile elements is lower in the Sun than in most of the solar twins (only one star has the same [X/Fe]-T C distribution as the Sun), but for many stars, the relation between [X/Fe] and T C is not well defined.

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“…Because it is so simple to use, ARES has been one of the most widely adopted codes for automatic EW measurements (e.g., Hekker & Meléndez 2007;Neves et al 2009;Sozzetti et al 2009;Ghezzi et al 2010;Ruchti et al 2011;Sousa et al 2011;Adibekyan et al 2012a;Tabernero et al 2012;Mortier et al 2013;Santos et al 2013;Monroe et al 2013;Maldonado et al 2013;Jofré et al 2014). ARES has also been used for asteroseismology studies that require stellar characterization (e.g.…”

Section: Introductionmentioning

confidence: 99%

ARES v2: new features and improved performance

Sousa

Santos

Adibekyan

et al. 2015

A&A

193

165

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Aims. We present a new upgraded version of ARES. The new version includes a series of interesting new features such as automatic radial velocity correction, a fully automatic continuum determination, and an estimation of the errors for the equivalent widths. Methods. The automatic correction of the radial velocity is achieved with a simple cross-correlation function, and the automatic continuum determination, as well as the estimation of the errors, relies on a new approach to evaluating the spectral noise at the continuum level. Results. ARES v2 is totally compatible with its predecessor. We show that the fully automatic continuum determination is consistent with the previous methods applied for this task. It also presents a significant improvement on its performance thanks to the implementation of a parallel computation using the OpenMP library.

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HIGH PRECISION ABUNDANCES OF THE OLD SOLAR TWIN HIP 102152: INSIGHTS ON Li DEPLETION FROM THE OLDEST SUN

Cited by 87 publications

References 35 publications

Seismic analysis of HD 43587Aa, a solar-like oscillator in a multiple system

Seismic analysis of HD 43587Aa, a solar-like oscillator in a multiple system

High-precision abundances of elements in solar twin stars

ARES v2: new features and improved performance

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