HD 174005: Another binary classified as<i>λ</i>Bootis

Faraggiana, R.; Gerbaldi, M.; Bonifacio, P.

doi:10.1051/0004-6361:20011440

Cited by 7 publications

(7 citation statements)

References 10 publications

(15 reference statements)

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“…The objects whose spectrum is tangled by that of one or more companions, according to our high resolution spectral inspection, are: HD 64 491 (Faraggiana & Gerbaldi 2003), HD 111 786 (Faraggiana et al 1997(Faraggiana et al , 2001a, HD 153 808 (Faraggiana et al 2001a), HD 174 005 (Faraggiana et al 2001b). This programme is going on; other stars have been recently found to be spectroscopic binaries, producing a composite spectrum that simulates that of a single λ Boo star; they will be discussed in a paper in preparation, together with the series of criteria selected for the duplicity detection.…”

Section: Binaries With Composite Spectramentioning

confidence: 85%

The heterogeneous class ofλBootis stars

Gerbaldi

Faraggiana²,

Lai³

2003

A&A

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Abstract. We demonstrate that it is arduous to define the λ Boo stars as a class of objects exhibiting uniform abundance peculiarities which would be generated by a mechanism altering the structure of their atmospheric layers. We collected the stars classified as λ Boo up to now and discuss their properties, in particular the important percentage of confirmed binaries producing composite spectra (including our adaptive optics observations) and of misclassified objects. The unexplained RV variables (and thus suspected binaries), the known SB for which we lack information on the companion, the stars with an UV flux inconsistent with their classification, and the fast rotating stars for which no accurate abundance analysis can be performed, are also reviewed.

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Section: Binaries With Composite Spectramentioning

confidence: 85%

The heterogeneous class ofλBootis stars

Gerbaldi

Faraggiana²,

Lai³

2003

A&A

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“…In addition to the stars for which high angular resolution observations have detected the duplicity and made it possible to measure the separation, we must consider those stars for which a detailed inspection of high resolution spectra revealed a composite spectrum: HD 64491 , HD 111786 (Faraggiana et al 2001a), HD 153808 (Faraggiana et al 2001a), HD 174005 (Faraggiana et al 2001b), as well as the four stars discussed in the previous sections (HD 11413, HD 79108, HD 196821 and HD 210111).…”

Section: Stars Classified As λ Boo With Composite Spectramentioning

confidence: 99%

$\mathsf{\lambda}$ Bootis stars with composite spectra

Faraggiana

Bonifacio

Caffau

et al. 2004

A&A

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Abstract.We examine the large sample of λ Boo candidates collected in Table 1 of Gerbaldi et al. (2003) to see how many of them show composite spectra. Of the 132 λ Boo candidates we identify 22 which definitely show composite spectra and 15 more for which there are good reasons to suspect a composite spectrum. The percentage of λ Boo candidates with composite spectra is therefore >17% and possibly considerably higher. For such stars the λ Boo classification should be reconsidered taking into account the fact that their spectra are composite. We argue that some of the underabundances reported in the literature may simply be the result of the failure to consider the composite nature of the spectra. This leads to the legitimate suspicion that some, if not all, the λ Boo candidates are not chemically peculiar at all. A thorough analysis of even a single one of the λ Boo candidates with composite spectra, in which the composite nature of the spectrum is duly considered, which would demonstrate that the chemical peculiarities persist, would clear the doubt we presently have that the stars with composite spectra may not be λ Boo stars at all.

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“…The hypothesis was advocated in a series of papers by the same authors (e.g. Faraggiana et al 2001), but was refuted in critical independent analyses (Stütz & Paunzen 2006;Griffin et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Gaia's view of the λ Boo star puzzle

Murphy

Paunzen

2016

Mon. Not. R. Astron. Soc.

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The evolutionary status of the chemically peculiar class of λ Boo stars has been intensely debated. It is now agreed that the λ Boo phenomenon affects A stars of all ages, from star formation to the terminal age main sequence, but the cause of the chemical peculiarity is still a puzzle. We revisit the debate of their ages and temperatures in order to shed light on the phenomenon, using the new parallaxes in Gaia Data Release 1 with existing Hipparcos parallaxes and multicolour photometry. We find that no single formation mechanism is able to explain all the observations, and suggest that there are multiple channels producing λ Boo spectra. The relative importance of these channels varies with age, temperature and environment.

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HD 174005: Another binary classified asλBootis

Abstract: Abstract. We demonstrate that HD 174005, a star recently classified as belonging to the λ Boo group, is in reality a double lined spectroscopic binary; at some phases, the observed composite spectrum may be similar to that of a single star with weak metal lines.

Cited by 7 publications

References 10 publications

The heterogeneous class ofλBootis stars

The heterogeneous class ofλBootis stars

$\mathsf{\lambda}$ Bootis stars with composite spectra

Gaia's view of the λ Boo star puzzle

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