Abundance analysis of two late A-type stars HD 32115 and HD 37594

Bikmaev, I.; Ryabchikova, T.; Bruntt, H.; Мусаев, Ф. А.; Mashonkina, L.; Belyakova, E. V.; Shimansky, V. V.; Barklem, P. S.; Галазутдинов, Г. А.

doi:10.1051/0004-6361:20020593

Cited by 34 publications

(55 citation statements)

References 41 publications

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“…Abundance calculations were performed in the LTE approximation by using 9 (Kurucz 1993; with modifications by V. Tsymbal and L. Mashonkina for PC, private communication). Atomic parameters of the spectral lines were extracted from the  data base with corrections of oscillator strengths in a few cases as described in the paper of Bikmaev et al (2002).…”

Section: "Classical" Abundance Analysis (Methods B)mentioning

confidence: 99%

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Bruntt¹,

Bikmaev

Catala

et al. 2004

A&A

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Abstract.One of the goals of the ground-based support program for the  and / satellite missions is to characterize suitable target stars for the part of the missions dedicated to asteroseismology. We present the detailed abundance analysis of nine of the potential  main targets using the semi-automatic software . For two additional  targets we could not perform the analysis due to the high rotational velocity of these stars. For five stars with low rotational velocity we have also performed abundance analysis by a classical equivalent width method in order to test the reliability of the  software. The agreement between the different methods is good. We find that it is necessary to measure abundances extracted from each line relative to the abundances found from a spectrum of the Sun in order to remove systematic errors. We have constrained the global atmospheric parameters T eff , log g, and [Fe/H] to within 70−100 K, 0.1−0.2 dex, and 0.1 dex for five stars which are slow rotators (v sin i < 15 km s −1 ). For most of the stars we find good agreement with the parameters found from line depth ratios, H α lines, Strömgren indices, previous spectroscopic studies, and also log g determined from the  parallaxes. For the fast rotators (v sin i > 60 km s −1 ) it is not possible to constrain the atmospheric parameters.

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Section: "Classical" Abundance Analysis (Methods B)mentioning

confidence: 99%

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Bruntt¹,

Bikmaev

Catala

et al. 2004

A&A

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“…The software is called VWA which has a graphical user interface (GUI). The method and the VWA software have been described in detail by Bruntt et al (2002Bruntt et al ( , 2004 and the method compared to the classical EW method by Bikmaev et al (2002). The abundance analysis relies on atomic parameters from the VALD database (Kupka et al 1999;Piskunov et al 1995) and uses modified ATLAS9 atmospheric models from interpolation in the grid published by Heiter et al (2002).…”

Section: Abundance Analysis: Methodsmentioning

confidence: 99%

Binarity, activity and metallicity among late-type stars

Dall¹,

Bruntt²,

Strassméier

2005

A&A

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We present the first in a series of papers that attempt to investigate the relation between binarity, magnetic activity, and chemical surface abundances of cool stars. In the current paper, we lay out and test two abundance analysis methods and apply them to two well-known, active, single stars, HD 27536 (G8IV-III) and HD 216803 (K5V), presenting photospheric fundamental parameters and abundances of Li, Al, Ca, Si, Sc, Ti, V, Cr, Fe, Co and Ni. The abundances from the two methods agree within the errors for all elements except calcium in HD 216803, which means that either method yields the same fundamental model parameters and the same abundances. Activity is described by the radiative loss in the Ca ii H and K lines with respect to the bolometric luminosity, through the activity index R HK . Binarity is established by very precise radial velocity (RV) measurements using HARPS spectra. The spectral line bisectors are examined for correlations between RV and bisector shape to distinguish between the effects of stellar activity and unseen companions. We show that HD 27536 exhibit RV variations mimicking the effect of a low-mass (m ∼ 4 M J ) companion in a relatively close (a ∼ 1 AU) orbit. The variation is strongly correlated with the activity, and consistent with the known photometric period P = 306.9 d, demonstrating a remarkable coherence between R HK and the bisector shape, i.e. between the photosphere and the chromosphere. We discuss the complications involved in distinguishing between companion and activity induced RV variations.

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“…Rasmussen et al (2002) and Bikmaev et al (2002). In the later paper we study two A-type stars and both have low v sin i (9 and 21 km s −1 ).…”

Section: Reliability Of Vwamentioning

confidence: 97%

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Bruntt

Catala

Garrido

et al. 2002

A&A

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Abstract.One of the goals of the ground-based support program for the COROT and MONS/Rømer satellite missions is to select and characterise suitable target stars for the part of the missions dedicated to asteroseismology. While the global atmospheric parameters may be determined with good accuracy from the Strömgren indices, careful abundance analysis must be made for the proposed main targets. This is a time consuming process considering the long list of primary and secondary targets. We have therefore developed new software called vwa for this task. The vwa automatically selects the least blended lines from the atomic line database vald, and consequently adjusts the abundance in order to find the best match between the calculated and observed spectra. The variability of HD 49434 was discovered as part of COROT ground-based support observations. Here we present a detailed abundance analysis of HD 49434 using vwa. For most elements we find abundances somewhat below the Solar values, in particular we find [Fe/H] = −0.13 ± 0.14. We also present the results from the study of the variability that is seen in spectroscopic and photometric time series observations. From the characteristics of the variation seen in photometry and in the line profiles we propose that HD 49434 is a variable star of the γ Doradus type.

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Abundance analysis of two late A-type stars HD 32115 and HD 37594

Cited by 34 publications

References 41 publications

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Abundance analysis of targets for the COROT/MONS asteroseismology missions

Binarity, activity and metallicity among late-type stars

Abundance analysis of targets for the COROT/MONS asteroseismology missions

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