Radial velocity determination by CCF using a synthetic spectrum as the template and detecting component spectra in SB1 binaries
Radial velocity determination is one of the basic methods of learning onstars and their systems. We aim at utilizing a computerized method forradial velocity measurements from spectra on electronic and photographicmedia. We compute the crosscorrelation function of an observed andsynthetic spectrum. Applicability of the method is documented onelectronic spectra of the double star V624 Her as well as photographicspectra of the binary AR Aur. The feasibility of the method fordetecting of component spectra is demonstrated on systems HD 861 and HD71973. We also show a possible way of using wide features such ashydrogen lines in early type stars in radial velocity determination.
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Abundance analysis of Am binaries and search for tidally driven abundance anomalies - II. HD861, HD18778, HD20320, HD29479, HD96528 and HD108651
The main goal of this paper is to continue a systematic abundanceanalysis of a sample of Am binaries in order to search for possibleabundance anomalies driven by tidal interaction in these binary systems.New CCD observations in two spectral regions (6400-6500 and 6660-6760Å) of HD861, HD18778, HD20320, HD29479, HD96528 and HD108651 wereobtained. Synthetic spectrum analysis was carried out, and basic stellarproperties, effective temperatures, gravities, projected rotationalvelocities, masses, ages and abundances of several elements weredetermined. We conclude that HD861, 29479 and 108651 are typical Amstars, while HD20320 and 96528 are mild Am stars. HD18778 turned out notto be an Am star although its projected rotational velocity is very low(27 kms-1). On the contrary, HD96528 has one of the highestprojected rotational velocities (85 kms-1) among Am binarieswith orbital periods in the range 20-200 d, and yet it exhibits Amanomalies. Pseudo-synchronization and abundance anomalies are discussedin the context of possible tidal effects.
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A search for SB2 systems among selected Am binaries
We report on the detection of secondary spectra in five spectroscopicbinary systems: HD 434, HD 861, HD 108642, HD 178449, and HD 216608.High signal-to-noise high resolution spectroscopic observations werecarried out at the Bulgarian NAO Rozhen as part of an extended projectconcerned mainly with Am stars in binary systems. Our knowledge aboutearly type binaries has serious gaps. This is true especially when it isonly based on older photographic techniques. We concluded thatphotographic data involving longer orbital periods (where Doppler shiftsdue to the orbital motion are comparable or even less than therotational broadening of the spectral lines) and early type stars (thathave only a few and usually broad lines) should be revisited or at leastused with caution. We demonstrate that for the five systems how CCDobservations made with 2-m class telescopes can discover the binarynature or secondary spectra of many currently unresolved SB1 systems.Important astrophysical information such as the atmospheric parametersand the mass ratios are used to unravel previous misinterpretations ofthe data leading often to spurious orbits.
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Discovery of the Secondary in the Spectrum of the SB1 System HD 861
We report the detection of the second spectrum in the SB1 system HD 861.The lines of the second spectrum are sharper than the primary spectrumand move in the opposite way as the lines of the primary. The mostprobable explanation is that they originate from the so far unseensecondary component of the binary system.
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Behaviour of calcium abundance in Am-Fm stars with evolution
Calcium abundance in the atmosphere of Am stars is examined as afunction of their evolutionary state within the main sequence. Newspectroscopic abundances as well as abundances obtained photometricallyby Guthrie (1987) are used, since they are mutually quite consistent.The main result of this work is that, contrary to earlier suggestions,calcium abundance does not tend to be larger in evolved Am stars than inunevolved ones, for objects distributed along a given evolutionary trackin the HR diagram. The trend appears to be the reverse, if it is presentat all. For our whole sample of Am stars, there is a significantcorrelation between calcium abundance and effective temperature, in thesense that the cooler objects are the most Ca-deficient, hence have themost pronounced Am peculiarity. This implies an apparent correlationbetween calcium deficiency and age, although the lack of Am starsyounger than log t = 8.6 seems real. Our results are fully consistentwith the low rate of Am stars observed in young clusters and withtheoretical predictions of time-dependent radiative diffusion (Alecian1996). Based on observations collected at Observatoire de Haute Provence(CNRS), France, and on data from the ESA HIPPARCOS astrometry satellite.
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On the nature of the AM phenomenon or on a stabilization and the tidal mixing in binaries. II. Metallicity and pseudo-synchronization.
We reveal sufficient evidences that for Am binaries the metallicitymight depend on their orbital periods, P_orb_, rather than on vsini. Inparticular, δm_1_ index seems to decrease with increasing orbitalperiod up to at least P_orb_=~50d, probably even up to P_orb_=~200d.This gives further support to our "tidal mixing + stabilization"hypothesis formulated in Part I. Moreover, while the most metallic Amstars seem to have rather large periods the slowest rotators are foundto exhibit substantially shorter P_orb_. A questioning eye is thus caston the generally adopted view that Am peculiarity is caused by asuppressed rotationally induced mixing in slowly rotating `single'stars. The observed anticorrelation between rotation and metallicity mayhave also other than the `textbook' explanation, namely being the resultof the correlation between metallicity and orbital period, as themajority of Am binaries are possibly synchronized. We further argue thatthere is a tendency in Am binaries towards pseudo-synchronization up toP_orb_=~35d. This has, however, no serious impact on our conclusionsfrom Part I; on the contrary, they still hold even if this effect istaken into account.
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On the nature of the AM phenomenon or on a stabilization and the tidal mixing in binaries. I. Orbital periods and rotation.
The paper casts a questioning eye on the unique role of the diffusiveparticle transport mechanism in explaining the Am phenomenon and arguesthat the so-called tidal effects might be of great importance incontrolling diffusion processes. A short period cutoff at =~1.2d as wellas a 180-800d gap were found in the orbital period distribution (OPD) ofAm binaries. The existence of the former can be ascribed to the state ofthe primaries with the almost-filled Roche lobes. The latter couldresult from the combined effects of the diffusion, tidal mixing andstabilization processes. Because the tidal mixing might surpassdiffusion in the binaries with the orbital periods P_orb_ less thanseveral hundred days and might thus sustain the He convection zone,which would otherwise disappear, no Am stars should lie below thisboundary. The fact that they are nevertheless seen there implies theexistence of some stabilization mechanism (as, e.g., that recentlyproposed by Tassoul & Tassoul 1992) for the binaries with orbitalperiods less than 180d. Further evidence is given to the fact that theOPD for the Am and the normal binaries with an A4-F1 primary arecomplementary to each other, from which it stems that Am stars are closeto the main sequence. There are, however, indications that they haveslightly larger radii (2.1-3 Rsun_) than expected for theirspectral type. The generally accepted rotational velocity cutoff at=~100km/s is shown to be of little value when applied on Am binaries ashere it is not a single quantity but, in fact, a function of P_orb_whose shape is strikingly similar to that of the curves of constantmetallicity as ascertained from observations. This also leads to thewell known overlap in rotational velocities of the normal and Am starsfor 402.5d.We have exploited this empirical cutoff function to calibrate thecorresponding turbulent diffusion coefficient associated with tidalmixing, having found out that the computed form of the lines of constantturbulence fits qualitatively the empirical shape of the curves ofconstant metallicity. As for larger orbital periods(20d55km/s found by Burkhart(1979) would then be nothing but a manifestation of insufficientlypopulated corresponding area of larger P_orb_.
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Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
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Programmes d'observation des binaires spectroscopiques et informations du 14ème catalogue complémentaire
Not Available
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The period distribution of unevolved close binary systems
Period distributions have been examined for various spectral types ofabout 600 (eclipsing and spectroscopic) close binaries, which are likelyto be substantially unevolved. The comparison with the previouscorresponding analyses of extensive (but heterogeneous) binary samplesallows a clarification of the extent of the evolutionary andobservational selection effects. Remarkably, this analysis reveals agreat deficiency of short period binaries (with periods corresponding tocase A mass transfer) in the whole spectral range. For the late spectraltypes, this result may be connected with postformation angular momentumloss caused by stellar wind magnetic braking; at least for the late Band A spectral range, a ready interpretation of this finding is thatclose binaries of corresponding periods and spectral types are rarelyformed.
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Lists of photometric AM candidates
The Geneva photometric m parameter (Nicolet and Cramer, 1982) is used inorder to select Am photometric candidates from the Rufener (1981)catalogue. Two lists are given, the first containing field stars and thesecond cluster stars. According to the photometric criteria thediffusion process probably responsible for the Am phenomenon takes placerather quickly as Am candidates are present in young clusters. It isconfirmed that the phenomenon is enhanced by low rotational velocity andhigh metallicity. The age seems to slightly affect the Am phenomenon.
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List of Estimated Angular Separations of Spectroscopic Binaries
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1981A&AS...44...47H&db_key=AST
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Properties of AM stars in the Geneva photometric system
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&A....92..289H&db_key=AST
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A comparison of the orbital inclinations of the spatially close spectroscopic double stars
The reported investigation takes into account 888 spectroscopicbinaries. It was possible to obtain 120 groups whose elements arespatially close according to the given definition. These 120 groupscontain 313 spectroscopic binaries. 136 of these binaries are 2-spectrumsystems, 177 are 1-spectrum systems, and 62 are eclipsing binaries. Thenumber of systems with known luminosity class is 54. The spectraldistribution of the 313 systems is discussed. The orbital inclinationsand other parameters are presented in a table.
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Seventh catalogue of the orbital elements of spectroscopic binary systems.
Not Available
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Catalogue of early-type stars measured in a narrow-band photometric system
A compilation of the photoelectric measurements in the Barbier-Morguleffsystem is presented. The catalogue includes data for 773 stars ofspectral type 08 to F6. 706 stars have been measured at least twice.
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Multicolor photometry of metallic-line stars. III. A photometric catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974RMxAA...1..175M&db_key=AST
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Catalogue of AM stars with known spectral types
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS...10..385H&db_key=AST
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Spectroscopic binaries - 12th complementary catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973A&AS...10..105P&db_key=AST
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Etude de la structure galactique a l'aide DU prisme-objectif : une region dans Cas.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&A....17..253M&db_key=AST
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Orbital elements of the spectroscopic binary HD 201359 - AGK2 +47 1705.
Abstract image available at:http://adsabs.harvard.edu/abs/1971A&A....15..304A
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Orbital elements of the spectroscopic binaries HD 24733 and HD 861.
Abstract image available at:http://adsabs.harvard.edu/abs/1971A&A....14..189A
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Catalogue des étoiles mesurées dans le système photométrique de l'Observatoire de Genève
Not Available
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Catalogue et bibliographie des étoiles A à spectre particulier - Deuxième supplément
Not Available
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Etude pour chaque champ de l'absorption et de la repartition des vitesses radiales EN fonction de la distance.
Not Available
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Catalogue et bibliographie des étoiles A à spectre particulier Premier supplément
Not Available
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Peculiar and Metallic-Line a - Stars in a Galactic Zone.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1959ApJ...129...88S&db_key=AST
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Mesures de vitesses radiales au spectrographe C de l'Observatoire de Haute Provence
Not Available
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La mesure des vitesses radiales auprisme objectif. VI. -Liste des vitesses radiales déterminées au prisme objectif à vision directe
Not Available
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