On the Variability of A3-F0 Luminosity Class III-V Stars
I investigate the Hipparcos Satellite photometry of A3-F0 stars ofluminosity classes III-V to learn about their variability and identify afew stars for which further study is desirable.
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New variable chemically peculiar stars identified in the HIPPARCOS archive
Since variability of chemically peculiar (CP) stars plays an importantrole for the astrophysical explanation of their outstanding behaviour,we have identified new variable CP stars listed in Renson's catalogueusing the extensive Hipparcos Variability Annex. From the 293 objectsfound, 33 were excluded because they are no CP stars and/or have noperiod listed, half of the remaining stars are newly identified and halfhad been already included in the catalogue of variable CP stars by\cite[Catalano & Renson (1997).]{Ca} Most of the newly identifiedvariability is due to an apparent magnetic field coupled with stellarrotation (oblique rotator model). The constraints of this model arefulfilled for all but three CP2 stars. Variations of bona fide Am-Fmstars are exclusively explained by eclipses of binary systems.Furthermore eight candidates of the >~mma Doradus group (pulsatingAm-Fm stars) were detected. Based on data from the ESA Hipparcosastrometry satellite. Table 1 is also available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) orvia\break http://cdsweb.u-strasbg.fr/Abstract.html
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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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The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle
The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
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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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The 71st Name-List of Variable Stars
Not Available
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Light curve of the ellipsoidal variable HD 1826.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1989CoSka..18...17B&db_key=AST
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Miscellaneous spectroscopic notes
Results of slit-spectrograph observations are reported for approximately260 stars. The data presented range from recognition of many new Ap, Am,and other unusual stars to H-alpha observations of early-typesupergiants and Be stars. The material discussed was obtained over thepast 40 years at a number of U.S. observatories and at the DominionAstrophysical Observatory in Victoria, B.C.
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Photometric variability of the binary HD 1826
Photoelectric two-color measurements of the single-line spectroscopicbinary HD 1826 are presented showing its photometric variability. Theperiod of the light variations has been found to be in excellentagreement with the orbital period derived from the radial velocitymeasurements. An estimation of the amplitude of the variations of 0.03mag has been obtained roughly independent of color. The system appearsto be an ellipsoidal variable and the available preliminary results arediscussed in light of the most probable binary model.
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Photometric variability of the binary HD 1826
Photoelectric two-color measurements of the single-lined spectroscopicbinary HD 1826 are presented, showing its photometric variability. Theperiod of the light variations has been found to be in excellentagreement with the orbital period from the radial-velocity measurements.An estimate of the amplitude of the variations of 0.03 magnitudes hasbeen obtained roughly independent of color. The system appears to be anellipsoidal variable, and the available preliminary results arediscussed in the light of the most probable binary model.
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The ellipsoidal variable stars
An annotated bibliography is presented for the ellipsoidal variableclass of noneclipsing close binaries, and a method is furnished for theanalysis of the light curves and spectroscopic data to determine thephysical parameters of such systems. Attention is given to confirmedellipsoidal variables, as well as suspected and rejected ones, and tothe characteristics of theoretical ellipsoidal light curves.
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The 67th Name-List of Variable Stars
Not Available
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Programmes d'observation des binaires spectroscopiques et informations du 14ème catalogue complémentaire
Not Available
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Four-colour and H-beta photometry of B stars in Fehrenbach and Burnage radial velocity fields at B about -30 deg
Observations in uvby and H-beta are presented for 39 stars classified asB-type in seven 4 x 4-deg fields studied by Fehrenbach and Burnage(1981, 1982) at b about -30 deg. About half the stars arephotometrically little-evolved B stars; most of the rest areintermediate A stars. Intrinsic color and absolute-magnitudecalibrations are applied: that of Hilditch et al. (1983) forintermediate A stars is estimated to be much less certain than those forother types. Maps of reddening along lines of sight indicate that littlereddening occurs within 100 pc of the sun, that essentially allreddening has occurred within z = + or - 150-200 pc, and that the totalreddening is essentially consistent with values given by the Bursteinand Heiles (1982) HI/GC method. The luminosities of some faint early Bstars cannot be usefully constrained by placing them within thereddening structure. One of the two program stars with very large radialvelocities is a horizontal branch object; the other has peculiar colors.
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A period-finding method for sparse randomly spaced observations of 'How long is a piece of string?'
A mathematical method for identifying the correct period of a variablestar from a small number of unequally spaced observations is presented.Previous methods using Fourier-transform and least-squares techniquesare reviewed. The true-string-length approach of Burke et al. (1970) isrefined by scaling the observations to place equal emphasis on theobservational and periodic members of the equation. It is shown that theminimum string length corresponding to a correct variable-star periodwill lie between 1.4 and 1.8. The effect of random error is considered,and criteria for predicting the number of false periods that will begenerated by the method are presented. The computational routine isdescribed. The method is demonstrated on several stars, and a new orbitis characterized for 17 Lyr, a spectroscopic binary observed by Abt andLevy (1976). An advantage of the method is seen in the fact that it canestimate the period of a variable after as few as 20 observations,allowing the timing of further observations to be planned efficiently.
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Five New Variable Stars
Not Available
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VRI photometry of selected SAO stars
Johnson V, R, and I photoelectric photometry has been obtained for 199SAO stars in support of the Near Infrared Photographic Sky Survey. Thesedata are utilized in the calibration of survey photographs and arepresented here to assist other programs reliant upon access tophotometry in the photographic infrared.
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Seventh catalogue of the orbital elements of spectroscopic binary systems.
Not Available
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A photometric study of SW Andromedae.
Abstract image available at:http://adsabs.harvard.edu/abs/1977PASP...89..699M
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Spectroscopic binaries with circular orbits.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971AJ.....76..544L&db_key=AST
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Spectrophotometry of VZ CANCRI
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1967ApJ...147..151D&db_key=AST
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