134 research outputs found
HD 174005: another binary classified as lambda Boo
We demonstrate that HD 174005, a star recently classified as belonging to the
lambda 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.Comment: Accepted by A&
Lambda Boo stars with composite spectra
We examine the large sample of lambda Boo candidates collected in Table 1 of
Gerbaldi et al. (2003) to see how many of them show composite spectra. Of the
132 lambda 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 lambda Boo candidates with composite spectra is
therefore > 17 and possibly considerably higher. For such stars the lambda 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 lambda Boo candidates are not chemically peculiar at all.
A thorough analysis of even a single one of the lambda 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 lambda Boo at all.Comment: Accepted for publication by A&A on June 3rd 200
C,N,O in lambda Boo stars and in composite spectra
The selective abundance of C, N, O (almost solar) with respect to that of
other elements (underabundant) in lambda Boo stars has been interpreted as a
characteristic peculiarity of these objects, when considered as single stars.
We show here that a similar selective abundance is predicted from the composite
spectra resulting from two unresolved stars in the same temperature range as
the lambda Boo stars.Comment: Accepted for publication on A&
A speckle interferometry survey of lambda Bootis stars
A search for duplicity of lambda Bootis stars has been made by using the
speckle camera installed at the Telescopio Nazionale Galileo. The operation
mode and the reduction procedure allow one to obtain not only the separation,
but also the magnitude difference between the components; the latter parameter
is fundamental for determining the degree of contamination from the secondary
component of a binary system and thus the importance of the veiling effect that
produces absorption lines weaker than normal. Two stars, HD 38545 and HD
290492, are close binaries with values of the separation and of the magnitude
difference such that only a composite spectrum can be observed. For another 15
lambda Bootis candidates, observed with negative results, the upper limits of a
possible companion separation are given.Comment: A&A in pres
Spectra of binaries classified as lambda Boo stars
High angular resolution observations have shown that some stars classified as
lambda Boo are binaries with low values of angular separation and magnitude
difference of the components; therefore the observed spectrum of these objects
is a combination of those of the two components. These composite spectra have
been used to define spectroscopic criteria able to detect other binaries among
stars classified as lambda Boo. The application of this method to HD 111786 is
presented: the contribution of 5 components to the observed spectrum is
demonstrated by the shape of the O I 7774 Angstrom feature. This result makes
unreliable any attempt to perform an abundance analysis of this object which
therefore must be definitely rejected from the class of the peculiar lambda Boo
stars. This approach allowed us also to recognize that the SB2 star HD 153808
is in reality a triple system.Comment: Accepted for publication by A&
The Solar Photospheric Nitrogen Abundance: Determination with 3D and 1D Model Atmospheres
We present a new determination of the solar nitrogen abundance making use of
3D hydrodynamical modelling of the solar photosphere, which is more physically
motivated than traditional static 1D models. We selected suitable atomic
spectral lines, relying on equivalent width measurements already existing in
the literature. For atmospheric modelling we used the co 5 bold 3D radiation
hydrodynamics code. We investigated the influence of both deviations from local
thermodynamic equilibrium (non-LTE effects) and photospheric inhomogeneities
(granulation effects) on the resulting abundance. We also compared several
atlases of solar flux and centre-disc intensity presently available. As a
result of our analysis, the photospheric solar nitrogen abundance is A(N) =
7.86 +/- 0.12.Comment: 6 pages, 4 figure
Chemical composition of a sample of bright solar-metallicity stars
We present a detailed analysis of seven young stars observed with the
spectrograph SOPHIE at the Observatoire de Haute-Provence for which the
chemical composition was incomplete or absent in the literature. For five
stars, we derived the stellar parameters and chemical compositions using our
automatic pipeline optimized for F, G, and K stars, while for the other two
stars with high rotational velocity, we derived the stellar parameters by using
other information (parallax), and performed a line-by-line analysis.
Chromospheric emission-line fluxes from CaII are obtained for all targets. The
stellar parameters we derive are generally in good agreement with what is
available in the literature. We provide a chemical analysis of two of the stars
for the first time. The star HIP 80124 shows a strong Li feature at 670.8 nm
implying a high lithium abundance. Its chemical pattern is not consistent with
it being a solar sibling, as has been suggested.Comment: To be published on A
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