The photospheric abundances of active binaries

Morel, Thierry; Micela, G.; Favata, F.; Katz, David

doi:10.1051/0004-6361:20041047

Cited by 27 publications

(39 citation statements)

References 54 publications

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“…From the mean abundances of our reference stars (Taylor 1999), we estimate an [Fe/ H] value that is slightly less than solar. This is in reasonable agreement with determinations by Fekel & Balachandran (1994), Morel et al (2004), and Randich et al (1993), who found ½Fe=H ¼ 0:0, À0.09, and À0.3, respectively.…”

Section: Spectral Type and Abundancesupporting

confidence: 93%

“…Thus, we classify it as a K0 III and conclude that its [Fe/ H] abundance is essentially solar. Our spectral type is in agreement with that given by Bidelman (1981) and Houk & Swift (1999), while our estimated iron abundance is in accord with ½Fe=H ¼ 0:0 found by Fekel & Balachandran (1994) and ½Fe=H ¼ À0:16 determined by Morel et al (2004).…”

Section: Spectral Type and Abundancesupporting

confidence: 93%

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Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

Fekel

Henry

2005

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We have obtained spectroscopy and photometry of three chromospherically active, single-lined spectroscopic binaries, HD 37824 (V1149 Ori), HD 181809 (V4138 Sgr), and HD 217188 (AZ Psc). HD 37824 has a circular orbit with a period of 53.57 days. Its primary is a K0 III star, while the secondary is likely a G or K dwarf. HD 181809 has an orbit with a period of 13.04667 days and a low eccentricity of 0.040. The primary has a spectral type of K0 III-IV, and its secondary is probably an M dwarf. The orbit of HD 217188 has a period of 47.1209 days and a moderately high eccentricity of 0.470. The spectral type of the primary is K0 III, while the secondary is likely an M dwarf. All three systems are estimated to have near solar iron abundances. Photometric observations spanning 15-16 years for all three stars yield mean photometric periods of 53.12, 59.85, and 90.89 days for HD 37824, HD 181809, and HD 217188, respectively. Thus, HD 37824 is rotating synchronously with the orbital period, while HD 181809 and HD 217188 are both rotating considerably slower than synchronously. All three stars show longterm variations in mean brightness and photometric amplitude, but no correlations are observed between the seasonal mean brightness, photometric amplitude, and seasonal photometric period in any of the stars. No clear evidence for long-term periodic variations in any of these parameters is present. The circular orbit of HD 37824 and the synchronous rotation of its K giant argue that the star is in the core helium-burning phase of its evolution. The giant components of HD 181809 and HD 217188 are asynchronous rotators, and both systems have eccentric orbits. Thus, those two stars are likely first-ascent giants.

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Section: Spectral Type and Abundancesupporting

confidence: 93%

Section: Spectral Type and Abundancesupporting

confidence: 93%

Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

Fekel

Henry

2005

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“…Further details can be found in Morel et al (2003Morel et al ( , 2004. As discussed in these papers, the selected transitions of the odd-Z elements (Sc, Co, and Ba) are not significantly broadened by hyperfine structure.…”

Section: Curve-of-growth Analysismentioning

confidence: 91%

Atmospheric parameters and chemical properties of red giants in the CoRoT asteroseismology fields

Morel

Miglio

Lagarde

et al. 2014

A&A

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A precise characterisation of the red giants in the seismology fields of the CoRoT satellite is a prerequisite for further in-depth seismic modelling. High-resolution FEROS and HARPS spectra were obtained as part of the ground-based follow-up campaigns for 19 targets holding great asteroseismic potential. These data are used to accurately estimate their fundamental parameters and the abundances of 16 chemical species in a self-consistent manner. Some powerful probes of mixing are investigated (the Li and CNO abundances, as well as the carbon isotopic ratio in a few cases). The information provided by the spectroscopic and seismic data is combined to provide more accurate physical parameters and abundances. The stars in our sample follow the general abundance trends as a function of the metallicity observed in stars of the Galactic disk. After an allowance is made for the chemical evolution of the interstellar medium, the observational signature of internal mixing phenomena is revealed through the detection at the stellar surface of the products of the CN cycle. A contamination by NeNa-cycled material in the most massive stars is also discussed. With the asteroseismic constraints, these data will pave the way for a detailed theoretical investigation of the physical processes responsible for the transport of chemical elements in evolved, low-and intermediate-mass stars.

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“…Moreover, as the star becomes cooler, the line blending becomes stronger, causing a possible [Fe/H] underestimation. An extensive study of the influence of stellar spots on deriving stellar parameters can be found, for instance, in Morel et al (2004). A possible influence of the atmospheric models used, optimal in the temperature window considered, cannot be discarded.…”

Section: [Fe/h] Correctionmentioning

confidence: 99%

Search for associations containing young stars (SACY)

Almeida

Santos

Melo³

et al. 2009

A&A

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The recently discovered coeval, moving groups of young stellar objects in the solar neighborhood represent invaluable laboratories for studying recent star formation and searching for high metallicity stars that can be included in future exo-planet surveys. In this study, we derived through an uniform and homogeneous method stellar atmospheric parameters and abundances for iron, silicium, and nickel in 63 post-T Tauri stars from 11 nearby young associations. We further compare the results with two different pre-main sequence (PMS) and main sequence (MS) star populations. The stellar atmospheric parameters and the abundances presented here were derived using the equivalent width of individual lines in the stellar spectra by assuming the excitation/ionization equilibrium of iron. Moreover, we compared the observed Balmer lines with synthetic profiles calculated for model atmospheres with a different line-formation code. We found that the synthetic profiles agree reasonably well with the observed profiles, although the Balmer lines of many stars are substantially filled-in, probably by chromospheric emission. Solar metallicity is found to be a common trend in all the nearby young associations studied. The low abundance dispersion within each association strengthens the idea that the origin of these nearby young associations is related to the nearby star-forming regions (SFR). Abundances of elements other than iron are consistent with previous results for Main Sequence stars in the solar neighborhood. The chemical characterization of the members of the newly found nearby young associations, performed in this study and intended to proceed in subsequent works, is essential to understanding and testing the context of local star formation and the evolutionary history of the galaxy.

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The photospheric abundances of active binaries

Cited by 27 publications

References 54 publications

Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

Atmospheric parameters and chemical properties of red giants in the CoRoT asteroseismology fields

Search for associations containing young stars (SACY)

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