Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components.

Ginestet, N.; Carquillat, J. M.

doi:10.1086/342942

Cited by 34 publications

(42 citation statements)

References 36 publications

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“…The primary is a late G-type giant, and the secondary could belong to the λ Bootis group (Griffin et al 1992). Its K-line type is earlier than derived from the hydrogen lines (Ginestet & Carquillat 2002). Therefore, this system is an excellent test for fitting isochrones of different metallicities.…”

Section: Discussionmentioning

confidence: 82%

Investigating the possible connection betweenλBootis stars and intermediate Population II type stars

Paunzen

Iliev

Fossati

et al. 2014

A&A

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Context. The λ Bootis stars are located at the upper main sequence of the Hertzsprung-Russell diagram and exhibit a peculiar abundance pattern. The light elements (C, N, O, and S) present solar abundances whereas all other elements are moderately to strongly underabundant. It has not yet been determined whether that abundance pattern is intrinsic, or is restricted to the stellar surface. Aims. If we follow the hypothesis that the λ Bootis stars are intrinsically metal-weak, then there should be a connection with the intermediate Population II and F-weak objects. Such a possible affinity has not been previously investigated. Methods. We present detailed elemental abundances, including those of the light elements carbon and oxygen, for 38 bright intermediate Population II and F-weak objects. In addition, we investigate the kinematic characteristics of the groups. Results. From photometric, spectroscopic, and kinematic data, there is no distinction between the intermediate Population II and F-weak type stars. We therefore conclude that the two groups are identical. However, it is possible to distinguish the λ Bootis stars from the intermediate Population II stars on the basis of elemental abundances, though not in terms of their kinematics. Conclusions. The λ Bootis stars seem to be distinct from the intermediate Population II group. Further asteroseismologic investigations and analyses of spectroscopic binary systems are needed to strengthen this conclusion.

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Section: Discussionmentioning

confidence: 82%

Investigating the possible connection betweenλBootis stars and intermediate Population II type stars

Paunzen

Iliev

Fossati

et al. 2014

A&A

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“…The bright giant Tr 91 (Trumpler 1938) in Mel 111 (Coma Berenices) is a well-known spectroscopic binary, classified as G7 III + A2.5 IV by Ginestet & Carquillat (2002). An orbit was published by Vinter Hansen (1940) and Abt & Willmarth (1999).…”

Section: Mel 111mentioning

confidence: 99%

Red giants in open clusters

Mermilliod¹,

Andersen

Latham

et al. 2007

A&A

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Context. The identification and characterisation of spectroscopic binaries with red-giant primaries in open clusters is important for a proper understanding of the colour-magnitude diagrams of the clusters. Moreover, the orbital eccentricities and axial rotations of these binaries are valuable probes into the inner structure and tidal interaction of the stars. Aims. We report on a comprehensive, long-term monitoring programme aiming to improve our knowledge of such binary systems. Methods. The radial velocities of 1309 red giants in 187 open clusters in the whole sky have been monitored with the Coravel and CfA spectrometers for 20 years, with a typical accuracy of 0.4 km s −1 per observation. Results. In total, 289 spectroscopic binaries were detected in the sample. We present first orbits for 67 systems and improved elements for another 64 previously published orbits, based on additional observations. For completeness, 25 published orbits are listed as well. The orbits are based on a total of 4039 observations, an average of 26 per system. Orbital periods range from 41.5 to 14 722 days (40 yrs), eccentricities from 0.00 to 0.81. The remaining 133 systems have too long periods, too few observations, and/or inadequate phase coverage for an orbit determination at this time.Conclusions. This paper provides a dramatic increase in the body of homogeneous orbital data available for red-giant spectroscopic binaries in open clusters. It will form the basis for a comprehensive discussion of membership, kinematics, and stellar and tidal evolution in the parent clusters.

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“…Hynek (1938) reports the composite classification F5 + A2 given in the Henry Draper Catalogue (here after HDC). Houk & SmithMoore (1988) propose A2/3 V + G8 III and GIN 2002 G8 III + A2.5: V. Let us remark that the spectral types given in the HDC for the cool components of composite spectrum stars are generally slightly misclassified, with a trend of giving a spectral type earlier than what is attributed by recent classifications (GIN 2002). The photometric model proposed by GIN 2002, based on G8 III + A2.5 V is consistent with the available data, including the Hipparcos parallax π = 2.11 ± 1.28 mas (ESA 1997) which has unfortunately a bad accuracy (σ π /π = 0.61).…”

Section: Notes On Individual Systemsmentioning

confidence: 92%

“…Ginestet et al (1997) classify the cool component of the system, G7: III, from a CCD spectrum obtained at OHP in the near infrared spectral region. Tentatively we can adopt G7 III + (A3)V for the classification of the system, given the available data and the statistical properties of such binaries (GIN 2002).…”

Section: Hde 255387-8 -Bd +19mentioning

confidence: 99%

Contribution to the study of composite spectra: XI. Orbital elements of some faint systems

Carquillat¹,

Prieur²

2007

Astron Nachr

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International audienceWe present the results of a radial-velocity study of nine new faint SB1 spectroscopic binaries with composite spectra: HD 137975-6, 177984, HDE 226489, 231613-4, 255387-8, 256138-9, 264997-8, 276787 and 293041-2. The observations were made at Haute-Provence and Cambridge observatories with CORAVEL instruments between 1982 and 2006. From the radial-velocity measurements of the cool components, we derive the orbital elements of those spectroscopic binaries for the first time. Using all the available data, we propose a model for each system that describes the nature of the individual components, with an estimation of the angular separation and orbital inclination. Finally we discuss the rotation-revolution synchronism of the cool components

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Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components.

Cited by 34 publications

References 36 publications

Investigating the possible connection betweenλBootis stars and intermediate Population II type stars

Investigating the possible connection betweenλBootis stars and intermediate Population II type stars

Red giants in open clusters

Contribution to the study of composite spectra: XI. Orbital elements of some faint systems

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