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The chemical composition of δ Scuti*
We present chemical abundances in the photosphere of δ Scuti(δ Sct) - a prototype of the class of pulsating variables -determined from the analysis of a spectrum obtained by using the 2-mtelescope at the Peak Terskol Observatory and a high-resolutionspectrometer with R= 52000, a signal-to-noise ratio 250 and fromInternational Ultraviolet Explorer spectra. The abundance pattern ofδ Sct consists of 49 chemical elements. The abundances of 19elements have not been investigated previously. The abundances of Pr andNd obtained from the lines of the second and third spectra are equal.The abundances of heavy elements indicate the overabundances withrespect to the solar system values up to 1 dex. The abundance pattern ofδ Sct is similar to the abundance patterns of Am-Fm or δ Deltype stars.A splitting of the cores of all clean lines is observed for the spectraof δ Sct and HD 57749. This can signify evidence of non-radialpulsations in these stars.
| Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of 14 000 F and G dwarfs
We present and discuss new determinations of metallicity, rotation, age,kinematics, and Galactic orbits for a complete, magnitude-limited, andkinematically unbiased sample of 16 682 nearby F and G dwarf stars. Our63 000 new, accurate radial-velocity observations for nearly 13 500stars allow identification of most of the binary stars in the sampleand, together with published uvbyβ photometry, Hipparcosparallaxes, Tycho-2 proper motions, and a few earlier radial velocities,complete the kinematic information for 14 139 stars. These high-qualityvelocity data are supplemented by effective temperatures andmetallicities newly derived from recent and/or revised calibrations. Theremaining stars either lack Hipparcos data or have fast rotation. Amajor effort has been devoted to the determination of new isochrone agesfor all stars for which this is possible. Particular attention has beengiven to a realistic treatment of statistical biases and errorestimates, as standard techniques tend to underestimate these effectsand introduce spurious features in the age distributions. Our ages agreewell with those by Edvardsson et al. (\cite{edv93}), despite severalastrophysical and computational improvements since then. We demonstrate,however, how strong observational and theoretical biases cause thedistribution of the observed ages to be very different from that of thetrue age distribution of the sample. Among the many basic relations ofthe Galactic disk that can be reinvestigated from the data presentedhere, we revisit the metallicity distribution of the G dwarfs and theage-metallicity, age-velocity, and metallicity-velocity relations of theSolar neighbourhood. Our first results confirm the lack of metal-poor Gdwarfs relative to closed-box model predictions (the ``G dwarfproblem''), the existence of radial metallicity gradients in the disk,the small change in mean metallicity of the thin disk since itsformation and the substantial scatter in metallicity at all ages, andthe continuing kinematic heating of the thin disk with an efficiencyconsistent with that expected for a combination of spiral arms and giantmolecular clouds. Distinct features in the distribution of the Vcomponent of the space motion are extended in age and metallicity,corresponding to the effects of stochastic spiral waves rather thanclassical moving groups, and may complicate the identification ofthick-disk stars from kinematic criteria. More advanced analyses of thisrich material will require careful simulations of the selection criteriafor the sample and the distribution of observational errors.Based on observations made with the Danish 1.5-m telescope at ESO, LaSilla, Chile, and with the Swiss 1-m telescope at Observatoire deHaute-Provence, France.Complete Tables 1 and 2 are only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/989
| The multiperiodicity of the gamma Doradus stars HD 224945 and HD 224638 as detected from a multisite campaign
We discuss new photometric data collected on the gamma Dor variables HD224945 and HD 224638. Multiperiodicity was detected in both stars,thanks to the clear spectral window of a multisite campaign thatinvolved five observatories. HD 224945 shows the shortest period amongthe gamma Dor stars, i.e., 0.3330 d. The pulsation behaviour is verydifferent: HD 224945 displays a set of frequencies spread over aninterval much larger than that of HD 224638. We clearly found evidencefor amplitude variations in the excited modes by comparing data fromdifferent years. HD 224945 and HD 224638 are among the best examples ofgamma Dor stars that show multimode pulsations, which make them veryinteresting from an asteroseismological point of view. Based onobservations partially collected at ESO-La Silla (Proposals 54.E-018 and56.E-0308).
| A database of high and medium-resolution stellar spectra
We present a database of 908 spectra of 709 stars obtained with theELODIE spectrograph at the Observatoire de Haute-Provence. 52 orders ofthe echelle spectra have been carefully fitted together to providecontinuous, high-resolution spectra in the wavelength range lambdalambda = 410-680 nm. The archive provides a large coverage of the spaceof atmospheric parameters: T_eff from 3700 K to 13 600 K, log g from0.03 to 5.86 and [Fe/H] from -2.8 to +0.7. At the nominal resolution,R=42 000, the mean signal-to-noise ratio is 150 per pixel. The spectragiven at this resolution are normalized to their pseudo-continuum andare intended to serve for abundance studies, spectral classification andtests of stellar atmosphere models. A lower resolution version of thearchive, at R=10 000, is calibrated in physical flux with a broad-bandphotometric precision of 2.5% and narrow-band precision of 0.5%. It iswell suited to stellar population synthesis of galaxies and clusters,and to kinematical investigations of stellar systems. The archive isdistributed in FITS format through the HYPERCAT and CDS databases. Basedon observations made on the 193 cm telescope at the Haute-ProvenceObservatory, France. Table 1 is only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/369/1048
| A revised catalogue of delta Sct stars
An extensive and up-dated list of delta Sct stars is presented here.More than 500 papers, published during the last few years, have beenrevised and 341 new variables have been added to our last list, sixyears ago. This catalogue is intended to be a comprehensive review onthe observational characteristics of all the delta Sct stars known untilnow, including stars contained in earlier catalogues together with othernew discovered variables, covering information published until January2000. In summary, 636 variables, 1149 references and 182 individualnotes are presented in this new list. Tables 1 and 2 will be accessibleonly in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Towards a seismic model of the delta Scuti star XX Pyxidis
Frequencies of 13 oscillation modes in the star XX Pyxidis (CD-24 7599)are accurately measured but for none of the modes the spherical harmonicdegree (l) is known. We present results of an attempt to construct themodel whose low-l mode frequencies reproduce possibly close theobservations. Models are constrained by the mean photometric andspectroscopic data for the star. However, the strongest constraint onthe effective temperture is from the requirement that the modes excitedin the star fall into the range of the modes driven by the opacitymechanism. Our models are built with the standard stellar evolution codeallowing no overshooting from the convective core. Effects of rotationare taken into account both in stellar evolution and in linearnonadiabatic oscillation calculations. Uniform rotation rate andconservation of the global angular momentum during evolution areassumed. We find several distinct mode identifications and associatedstellar models leading to frequency fits of similar quality.Determination of the l values for some of the modes could remove theambiguity. None of the fits is satifactory: the mean departures exceedthe mean observational frequency error by at least one order ofmagnitude. The fits could be improved by means of adjusting modelparameters that were kept fixed. However, such effort will be meaningfulonly after improving accuracy in calculation of the effects of rotationin oscillation frequencies.
| The most resonant pulsation frequency of delta Scuti stars
Pulsation of the Sun with a period of P0 ~ 160 min discoveredabout two decades ago, is still waiting explanation. In view of thehypothesis about its cosmological origin, and attempting to findsignature of this \p\ periodicity among other (short--period variable)stars, the pulsation frequencies of \del stars are subjected to specificanalysis. With a confidence level ~ 3.8sigma it is found that thefrequency nu_ {0} be the most ``resonant'' one for the total sample of318 pulsating stars of del type (the most commensurable, or``synchronizing'', period for all these stars occurs to be 162 \pm 4min). We conjecture that a) the p \ oscillation might be connected withperiodic fluctuations of gravity field (metrics), and b) the primaryexcitation mechanism of pulsations of del stars, reflected by this``ubiquitous'' p \ resonance, must be attributed perhaps to superfastrotation of their inner cores (their rates tend to be in near--resonancewith the ``universal'' \nu0$ frequency). The arguments aregiven favouring a cosmological nature of the \p\ oscillation.
| The stability of the frequency content in the light curves of the δ Scuti stars HD16439=V663 Cassiopeiae, AZ Canis Minoris, HD 223480=BF Phoenicis.
Within the frame of the study of the pulsational behaviour of δSct stars, multicolour photometry of (previously) consideredmonoperiodic or double mode pulsators was undertaken. The frequencycontent of the light variation of SAO 4710=HD 16439=V663 Cas is clearlychanging as a new frequency, not present in 1989, was observed in 1995;a slight decrease is also observed in the amplitude of the dominantterm. The light curve of V663 Cas is now explained by three frequencies,but the residual noise probably masks other terms. SAO 231800=HD223480=BF Phe is confirmed to be a monoperiodic δ Sct star, butcomparing the 1989 and 1993 photometric measurements a strong reductionin the b amplitude is observed; on the other hand, the V amplituderemained stable in 1991 and 1993. The monoperiodic light curve of HR2989=AZ CMi seems more stable, giving only slight hints that smallchanges occurred. The different photometric behaviours of these starsare discussed, also by comparing them with other monoperiodic pulsators(β Cas, 28 And, τ Peg).
| BH Piscium=HD 224639: a δ Scuti star with a rich pulsation spectrum and changing mode amplitudes.
New B and V observations of the δ Scuti star BH Psc (64 hoursduring 13 quasi-consecutive nights in October and November 1994),combined with the previous ones obtained in 1991, have allowed us to getan improved resolution of its light curve, confirming the presence of alarge number (at least 13) of excited modes. There is strong evidencethat some modes have large amplitude variations over timescales shorterthan a few years, while others seem to be rather stable. There is alsoevidence that the pulsation energy in 1994 was lower than in 1991. Theratios between the amplitudes of the light and colour curves and theirphase shifts, available for the first time, tend to suggest the presenceof excited modes with l<=2.
| The complex photometric behaviour of the δ Scuti star HD 224639.
HD 224639 was photometrically observed for 20h in 1989 and 120h in 1991(454 and 2567 datapoints, respectively). The star shows a very complexpulsational content with 3 components with semi-amplitudes of about15mmag and many other terms with a smaller semi-amplitude. The 1991dataset allowed us to single out 11 components in the frequency rangebetween 5 and 12 c/d, but many more are probably present since theresidual rms of the fit is 8.6mmag, while the noise level is expected tobe 3.7mmag. By subdividing the 1991 dataset into two parts and bycomparing the results of the frequency analysis with those obtained fromthe 1989 dataset we found independent evidence in support of thereliability of four frequencies: 6.21, 8.49, 9.54 and 11.42 c/d. Sincemost of the 11 components are nonradial modes, their identification ishampered by the high rotational velocity (vsin i=110km/s) which veryprobably produces the splitting of an l mode into a multiplet(-l<=m<=+l) and, in any case, causes an appreciable shift infrequency of the central value (m=0).
| A catalogue of variable stars in the lower instability strip.
Identifications, positions, photometry, spectra, some pulsationalfeatures, other astrophysical parameters and literature for 302pulsating variable stars in the lower instability strip, near the ZAMS,are given. About 185 stars have near homogeneous photometric informationin the Stroemgren's uvby-β photometric system. Thiscatalogue/database covers information published until November 1993.
| Main Sequence Variables
The pulsators along and near the main sequence are well-suited forasteroseismology and provide a probe of the stellar interior and itschanges with evolution. With the exception of rapidly oscillating Apstars (roAp), the pulsation periods range from 0.5 h to days. Thisrequires multisite campaigns lasting several weeks. The delta Scuti,roAp and beta Cephei variables offer the greatest potential, while thelonger-period g-mode pulsators (SPB -- slowly pulsating B stars -- andgamma Doradus variables) are very difficult to study. A summary of themultiperiod structure of delta Scuti stars is given. The twobest-studied stars, FG Vir and CD--24(deg) 7599, both have been WETtargets. A preliminary analysis of the 1995 campaign of FG Vir hasalready detected 19 frequencies. The standard photometric WET techniquehas a high duty cycle since the variable star is observed continuouslywith one channel. The study of main sequence variables requiresphotometric stability at low frequencies. The extension of the WETtechnique to low frequencies and its modification are discussed.
| δ Scuti stars: a new revised list
An extensive and up to date list of δ Sct stars is presented. Thiscatalogue is intended to be a comprehensive review of observationalcharacteristics of all the δ Sct stars known until now, includingstars contained in earlier catalogues together with other new discoveredvariables, covering information published until November 1993. Globalinformation in the form of histograms and diagrams are also shown.
| Insight into the Pulsational Behaviour of δ Scuti Stars
Not Available
| The 71st Name-List of Variable Stars
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| Doing research with small telescopes : frequency analysis of multiperiodic delta Scuti stars.
Not Available
| Light Variability of HD 224639, HD 224638 and HD 224945
Not Available
| Appulses and occultations of SAO stars by Mercury - 1987-1995
While no readily observable occultations were found in the presentpredictions for 78 close approaches by Mercury to stars in theSmithsonian Astrophysical Observatory catalog (1966) over the periodJanuary 1, 1987-December 31, 1995, seven occultations of stars withvisual magnitudes of 7 or fainter are noted. These events are presentedwith a view to searches for material in the vicinity of Mercury, as wellas investigations requiring close, bright stars for the improvement ofground-based Mercury images.
| Photometric variability of some early-type stars
Photometric observations of 12 variable early type stars are presented.The properties of individual stars are discussed, and an attempt is madeto interpret their variability. The information presented on the starsincludes the HD number and other identification, the observing runs, theperiodicity of the variations, an error estimate, and a tentativeclassification of each star.
| Nouvelle recherche de periodes d'etoiles Ap observees a ESO-VII
Not Available
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| Takýmyýldýz: | Baliklar |
| Sað Açýklýk: | 23h59m31.32s |
| Yükselim: | -02°50'37.6" |
| Görünürdeki Parlaklýk: | 7.128 |
| Uzaklýk: | 151.745 parsek |
| özdevim Sað Açýklýk: | 23.1 |
| özdevim Yükselim: | 4.8 |
| B-T magnitude: | 7.499 |
| V-T magnitude: | 7.159 |
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