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Non-radial pulsations in the γ Doradus star HD 195068
We present high resolution spectroscopic observations of the γDoradus star HD 195068. About 230 spectra werecollected over 2 years. Time series analysis performed on radialvelocity data shows a main peak at 1.61 d-1 , a frequency notyet detected in photometry. The Hipparcos photometric 1.25d-1 frequency is easily recovered as is 1.30 d-1while the third photometric frequency, 0.97 d-1 , is onlymarginally present. The good quality of our data, which includes 196spectra collected over seven consecutive nights, shows that both the1.61 d-1 and intermediate 1.27 d-1 (mixture of1.25 and 1.30 d-1 ) frequencies are present in the lineprofile variations. Using the Fourier-Doppler Imaging (FDI) method, thevariability associated with 1.61 d-1 can be successfullymodeled by a non-radial pulsation mode ℓ=5± 1, |m|=4±1. For the intermediate frequency 1.27 d-1 we deduceℓ=4± 1, |m|=3± 1. Evidence that the star is notpulsating in the radial mode (ℓ=0) rules out a previousclassification as an RR Lyrae type star. We investigate the timevariability of FDI power spectra concluding that the observed temporalvariability of modes can be explained by a beating phenomenon betweenclosely spaced frequencies of two non-radial modes. The distribution ofthe oscillation power within the line profile indicates that there is asignificant tangential velocity component of oscillations characteristicof high radial order gravity modes which are predicted to be observed inγ Doradus type stars.
| Fundamental parameters of Be stars located in the seismology fields of COROT
In preparation for the COROT space mission, we determined thefundamental parameters (spectral type, temperature, gravity, V sin i) ofthe Be stars observable by COROT in its seismology fields (64 Be stars).We applied a careful and detailed modeling of the stellar spectra,taking into account the veiling caused by the envelope, as well as thegravitational darkening and stellar flattening due to rapid rotation.Evolutionary tracks for fast rotators were used to derive stellar massesand ages. The derived parameters will be used to select Be stars assecondary targets (i.e. observed for 5 consecutive months) and short-runtargets of the COROT mission. Furthermore, we note that the main part ofour stellar sample falls in the second half of the main sequence lifetime, and that in most cases the luminosity class of Be stars isinaccurate in characterizing their evolutionary status.
| High precision determination of the atmospheric parameters and abundances of the COROT main targets
Context: .One of the main goals of the COROT mission is to get precisephotometric observations of selected bright stars in order to allow themodelling of their interior through asteroseismology. However, in orderto interpret the asteroseismological data, the effective temperature,surface gravity, and chemical composition of the stars must be knownwith sufficient accuracy.Aims.To carry out this task, we have developeda spectroscopic method called APASS (Atmospheric Parameters andAbundances from Synthetic Spectra) which allows precise analysis ofstars with a moderate to high rotational velocity, which is the case formost primary COROT targets.Methods.Our method is based on syntheticspectra in which individual lines are replaced by analysis units(isolated lines or line blends, depending on the crowding of thespectral region and on the rotational broadening). It worksdifferentially with respect to the Sun and allows the atmosphericparameters and chemical abundances to be determined by consideringanalysis units with different sensitivities to these variousparameters.Results.Using high signal-to-noise spectra and the APASSmethod, we determined the atmospheric parameters and chemical abundancesof 13 primary COROT targets. Our results agree well with those obtainedby Bruntt using his software VWA and with those obtained with thesoftware TEMPLOGG. However, in both cases, our error bars aresignificantly smaller than those of other methods. Our effectivetemperatures are also in excellent agreement with those obtained withthe IR photometry method. For five stars with relatively low rotationalvelocity, we also performed an analysis with a classicalequivalent-width method to test agreement with APASS results. We showthat equivalent-width measurements by Gaussian or Voigt profile-fittingare sensitive to the rotational broadening, leading to systematic errorswhenever the projected rotation velocity is non-negligible. The APASSmethod appears superior in all cases and should thus be preferred.
| Interferometric Observations of V838 Monocerotis
We have used long-baseline near-IR interferometry to resolve thepeculiar eruptive variable star V838 Mon and to provide the first directmeasurement of its angular size. Assuming a uniform disk model for theemission, we derive an apparent angular diameter at the time ofobservations (2004 November-December) of 1.83+/-0.06 mas. For a nominaldistance of 8+/-2 kpc, this implies a linear radius of 1570 +/- 400Rsolar. However, the data are somewhat better fitted byelliptical disk or binary component models, and we suggest that theemission may be strongly affected by ejecta from the outburst.
| Preparing the COROT Space Mission: New Variable Stars in the Galactic Anticenter Direction
The activities related to the preparation of the asteroseismic,photometric space mission COROT are described. Photoelectricobservations, wide-field CCD photometry, uvbyβ calibrations, andfurther time series have been obtained at different observatories andtelescopes. They have been planned to complete the COROT program in thedirection of the Galactic anticenter. In addition to suitableasteroseismic targets covering the different evolutionary stages betweenzero-age main sequence and terminal-age main sequence, we discoveredseveral other variable stars, both pulsating and geometric. We comparedresults on the incidence of variability in the Galactic center andanticenter directions. Physical parameters have been obtained, andevolutionary tracks fitting them have been calculated. The peculiaritiesof some individual stars are pointed out.Based on observations collected at the San Pedro Martír, SierraNevada, Teide, La Silla, Haute-Provence, and Roque de Los Muchachos(Telescopio Nazionale Galileo and Mercator telescopes) observatories.
| Abundance analysis of targets for the COROT/MONS asteroseismology missions. II. Abundance analysis of the COROT main targets
One of the goals of the ground-based support program for the COROT andMONS/RÖMER satellite missions is to characterize suitable targetstars for the part of the missions dedicated to asteroseismology. Wepresent the detailed abundance analysis of nine of the potential COROTmain targets using the semi-automatic software VWA. For two additionalCOROT targets we could not perform the analysis due to the highrotational velocity of these stars. For five stars with low rotationalvelocity we have also performed abundance analysis by a classicalequivalent width method in order to test the reliability of the VWAsoftware. The agreement between the different methods is good. We findthat it is necessary to measure abundances extracted from each linerelative to the abundances found from a spectrum of the Sun in order toremove systematic errors. We have constrained the global atmosphericparameters Teff, 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 agreementwith the parameters found from line depth ratios, H α lines,Strömgren indices, previous spectroscopic studies, and also log gdetermined from the HIPPARCOS parallaxes. For the fast rotators (v sin i> 60 km s-1) it is not possible to constrain theatmospheric parameters.Based on observations obtained with the 193 cm telescope at Observatoirede Haute Provence, France.
| Multi-site, multi-technique survey of γ Doradus candidates. I. Spectroscopic results for 59 stars
We present the first results of a 2-year high-resolution spectroscopycampaign of 59 candidate γ Doradus stars which were mainlydiscovered from the HIPPARCOS astrometric mission. More than 60% of thestars present line profile variations which can be interpreted as due topulsation related to γ Doradus stars. For all stars we alsoderived the projected rotation velocity (up to more than 200 kms-1). The amplitude ratios 2K/Δ m for the mainHIPPARCOS frequency are in the range 35-96 kms-1,mag-1. About 50% of the candidates arepossible members of binary systems, with 20 stars being confirmedγ Doradus. At least 6 stars present composite spectra, and in allbut one case (for which only one spectrum could be obtained), the narrowcomponent shows line profile variations, pointing towards anuncomfortable situation if this narrow component originates from a shellsurrounding the star. This paper is the first of a series concerningmode identification using both photometric and spectroscopic methods forthe confirmed γ Doradus stars of the present sample.Partially based on observations obtained at the Observatoire deHaute-Provence.
| Differential rotation in rapidly rotating F-stars
We obtained high quality spectra of 135 stars of spectral types F andlater and derived ``overall'' broadening functions in selectedwavelength regions utilizing a Least Squares Deconvolution (LSD)procedure. Precision values of the projected rotational velocity v \siniwere derived from the first zero of the Fourier transformed profiles andthe shapes of the profiles were analyzed for effects of differentialrotation. The broadening profiles of 70 stars rotating faster than v\sini = 45 km s-1 show no indications of multiplicity nor ofspottedness. In those profiles we used the ratio of the first two zerosof the Fourier transform q_2/q_1 to search for deviations from rigidrotation. In the vast majority the profiles were found to be consistentwith rigid rotation. Five stars were found to have flat profilesprobably due to cool polar caps, in three stars cuspy profiles werefound. Two out of those three cases may be due to extremely rapidrotation seen pole on, only in one case (v \sini = 52 km s-1)is solar-like differential rotation the most plausible explanation forthe observed profile. These results indicate that the strength ofdifferential rotation diminishes in stars rotating as rapidly as v \sini>~ 50 km s-1.Table A.1 is only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/412/813Based on observations collected at the European Southern Observatory, LaSilla, 69.D-0015(B).
| Rotation in Globular Cluster stars. Turn-off and subgiant stars in NGC 104, NGC 6397 and NGC 6752
We present a derivation of upper limits to the rotation of Main Sequencestars in three globular clusters using spectra obtained during timeallocated to the ESO Large Programs 165-L0263 and 167.D-0173, with UVESat VLT2 (Kueyen). The stars analyzed in this work do not show anyevidence of high values of rotational velocities as far as the outerlayers are concerned, in particular robust estimates for the upperlimits of the values of the mean projected rotational velocities areplaced, about /line{vrot sin i} = 3.5+/- 0.2 kms-1 and about /line{vrot sin i}=4.7+/-0.2 kms-1 for, respectively, the program turn-off and subgiantstars. On the basis of statistical considerations, assuming thatinclination of the rotational axis i is randomly oriented, and that allstars within the same group rotate at the same rate, we obtain estimatesfor the values of the true rotational velocities. These values are upperlimits to the true rotational velocities if there is some star-to-starscatter in rotational or macro-turbulent velocities. The mean values ofthese upper limits for vrot for the stars of the samespectral type averaged over the three clusters are found to berespectively, /line{v}rot<=3.5+/-0.4 km s-1 and/line{v}rot<=2.6+/-1.1 km s-1. Thus, theexplanation for the large rotational velocities found for the HorizontalBranch stars must be looked for either in the rotation of the core notdetectable in the outer layers (Sills & Pinsennault \cite{sill}) orin the acquisition of angular momentum during their evolution.Based on observations collected at the European Southern Observatory,Chile.
| The status of Galactic field λ Bootis stars in the post-Hipparcos era
The λ Bootis stars are Population I, late B- to early F-typestars, with moderate to extreme (up to a factor 100) surfaceunderabundances of most Fe-peak elements and solar abundances of lighterelements (C, N, O and S). To put constraints on the various existingtheories that try to explain these peculiar stars, we investigate theobservational properties of λ Bootis stars compared with areference sample of normal stars. Using various photometric systems andHipparcos data, we analyse the validity of standard photometriccalibrations, elemental abundances, and Galactic space motions. Therecrystallizes a clear picture of a homogeneous group of Population Iobjects found at all stages of their main-sequence evolution, with apeak at about 1 Gyr. No correlation of astrophysical parameters such asthe projected rotational velocities or elemental abundances with age isfound, suggesting that the a priori unknown mechanism, which createsλ Bootis stars, works continuously for late B- to early F-typestars in all stages of main-sequence evolution. Surprisingly, the sodiumabundances seem to indicate an interaction between the stars and theirlocal environment.
| Rotation of stars in NGC 6134. A comparison of delta Scuti stars and non-variable stars
We present results of spectroscopic observations of selected stars inthe southern open cluster NGC 6134. We have determined the rotationalvelocities of the six known delta Scuti stars in NGC 6134 as well asseveral other non-variable stars with similar colour temperature inorder to investigate if v sin i and variability is somehow connected: wefind no such correlation. We also compare the distribution of v sin i ofdelta Scuti stars and non-variable stars with four other well-studiedopen clusters to look for any systematic behaviour, but we find noconclusive evidence for v sin i and variability to be connected. We havealso used the spectra to carry out an abundance analysis of the deltaScuti stars in NGC 6134 to confirm the high metal content of thecluster. We find [Fe/H] = +0.38+/-0.05 which is in agreement with theresult obtained from Strömgren photometry. We also present Delta aphotometry of the cluster, but we find no chemical peculiar stars basedon this index. Based in part on observations obtained at the EuropeanSouthern Observatory at La Silla and UTSO-Las Campanas, Chile.
| Abundance analysis of targets for the COROT/MONS asteroseismology missions. I. Semi-automatic abundance analysis of the gamma Dor star HD 49434
One of the goals of the ground-based support program for the COROT andMONS/Römer satellite missions is to select and characterisesuitable target stars for the part of the missions dedicated toasteroseismology. While the global atmospheric parameters may bedetermined with good accuracy from the Strömgren indices, carefulabundance analysis must be made for the proposed main targets. This is atime consuming process considering the long list of primary andsecondary targets. We have therefore developed new software called VWAfor this task. The VWA automatically selects the least blended linesfrom the atomic line database VALD, and consequently adjusts theabundance in order to find the best match between the calculated andobserved spectra. The variability of HD 49434 was discovered as part ofCOROT ground-based support observations. Here we present a detailedabundance analysis of HD 49434 using VWA. For most elements we findabundances somewhat below the Solar values, in particular we find [Fe/H]= -0.13 +/- 0.14. We also present the results from the study of thevariability that is seen in spectroscopic and photometric time seriesobservations. From the characteristics of the variation seen inphotometry and in the line profiles we propose that HD 49434 is avariable star of the gamma Doradus type. Based on observations obtainedat Observatoire d'Haute Provence, France and at the Observatory ofSierra Nevada, Granada, Spain.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Exploration of the BaSeL stellar library for 9 F-type stars COROT potential targets. Comparisons of fundamental stellar parameter determinations
The Basel Stellar Library (BaSeL models) is constituted of the mergingof various synthetic stellar spectra libraries, with the purpose ofgiving the most comprehensive coverage of stellar parameters. It hasbeen corrected for systematic deviations detected in respect toUBVRIJHKLM photometry at solar metallicity, and can then be consideredas the state-of-the-art knowledge of the broad band content of stellarspectra. In this paper, we consider a sample of 9 F-type stars withdetailed spectroscopic analysis to investigate the Basel Stellar Libraryin two photometric systems simultaneously, Johnson (B-V, U-B) andStrömgren (b-y, m1, and c1). The samplecorresponds to potential targets of the central seismology programme ofthe COROT space experiment, which have been recently observed at OHP.The atmospheric parameters Teff, [Fe/H], and log g obtainedfrom the BaSeL models are compared with spectroscopic determinations aswell as with results of other photometric calibrations. For a carefulinterpretation of the BaSeL solutions, we computed confidence regionsaround the best chi 2-estimates and projected them onTeff-[Fe/H], Teff-log g, and log g-[Fe/H]diagrams. We first derive the 3 atmospheric parameters from the fullphotometric information available (Johnson and Strömgren data). TheBaSeL library has only been calibrated for broad band UBVRIJHKLMphotometry, and it presents therefore intrinsic limitations in respectto other photometric systems, especially with different bandwidth. Thus,using this combination (Johnson and Strömgren), BaSeL temperaturesare systematically lower ( ~ 130 K), and the discrepancy for the gravityand the metallicity can be quite large in comparison to the othermethods. To disentangle these unexpected discrepancies, we fixed thetemperatures at their spectroscopic values and studied the relativeinfluence of each colour index in the log g-[Fe/H] diagrams. We findinconsistent results between Strömgren and Johnson syntheticcolours. While the Johnson colours give impressively good log g-[Fe/H]solutions, the combination of the m1 and c1Strömgren synthetic indices does not provide reliable results. Thisis not, of course, due to any intrinsic superiority of the UBV over theStrömgren system, but to the properties of the BaSeL models.Finally, in order to simultaneously and accurately determine the stellarparameters Teff, [Fe/H] and log g, we suggest to use thecombination of the synthetic BaSeL indices B-V, U-B and b-y rather thanB-V, U-B, b-y, m1 and c1. Based on observationsmade on the 193~cm telescope at Observatoire de Haute-Provence, Franceand data from the ESA Hipparcos satellite. Figures 2-5, 7 and 8 are onlyavailable in electronic form at http://www.edpsciences.org
| Radial velocities of HIPPARCOS southern B8-F2 type stars
Radial velocities have been determined for a sample of B8-F2 type starsobserved by the Hipparcos satellite. Observations were obtained withinthe framework of an ESO key-program. Radial velocities have beenmeasured using a cross-correlation method, the templates being a grid ofsynthetic spectra. The obtained precision depends on effectivetemperature and projected rotational velocity of the star as well as ona possible asymmetry of the correlation peak generally due to secondarycomponents. New spectroscopic binaries have been detected from theseasymmetries and the variability of the measured radial velocity.Simulations of binary and triple systems have been performed. Forbinaries our results have been compared with Hipparcos binary data.Adding the variable radial velocities, the minimum binary fraction hasbeen found 60% for physical systems. Radial velocities have beendetermined for 581 B8-F2 stars, 159 being new. Taking into accountpublished radial velocities, 39% south A-type stars with V magnitudelower than 7.5 have a radial velocity. Based on observations obtained atthe European Southern Observatory (ESO, La Silla, Chile) and on datafrom the ESA Hipparcos astrometry satellite.}\fnmsep \thanks{Tables 7, 8and 9 are only available in electronic form at the CDS via anonymous ftpto cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars
We present X-ray data for all main-sequence and subgiant stars ofspectral types A, F, G, and K and luminosity classes IV and V listed inthe Bright Star Catalogue that have been detected as X-ray sources inthe ROSAT all-sky survey; several stars without luminosity class arealso included. The catalogue contains 980 entries yielding an averagedetection rate of 32 percent. In addition to count rates, sourcedetection parameters, hardness ratios, and X-ray fluxes we also listX-ray luminosities derived from Hipparcos parallaxes. The catalogue isalso available in electronic form via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| An extensive Delta a-photometric survey of southern B and A type bright stars
Photoelectric photometry of 803 southern BS objects in the Deltaa-system as detection tool for magnetic chemically peculiar (=CP2) starshas been carried out and compared to published spectral types. Thestatistical yield of such objects detected by both techniques ispractically the same. We show that there are several factors whichcontaminate the search for these stars, but this contamination is onlyof the order of 10% in both techniques. We find a smooth transition fromnormal to peculiar stars. Our sample exhibits the largest fraction ofCP2 stars at their bluest colour interval, i.e. 10% of all stars in thecolour range -0.19 <= B-V < -0.10 or -0.10 <= b-y < -0.05.No peculiar stars based on the Delta a-criterion were found at bluercolours. Towards the red side the fraction of CP2 stars drops to about3% for positive values of B-V or b-y with red limits roughlycorresponding to normal stars of spectral type A5. The photometricbehaviour of other peculiar stars: Am, HgMn, delta Del, lambda Boo, Heabnormal stars, as well as Be/shell stars and supergiants shows someslight, but definite deviations from normal stars. Spectroscopic andvisual binaries are not distinguished from normal stars in their Delta abehaviour. The results of this work justify larger statistical work(e.g. in open clusters) employing more time-saving photometric methods(CCD). \newpage Based on observations obtained at the European SouthernObservatory, La Silla, Chile. This research has made use of the Simbaddatabase, operated at CDS, Strasbourg, France. Table 2 is only availablein electronic form via anonymous ftp 130.79.128.5 orhttp://cdsweb.u-strasbg.fr/Abstract.html
| UBV polarimetry of 361 A- and F-type stars in selected areas
We present simultaneous UBV linear polarization measurements for 361 A-and F-type stars with accurate colour excess and distance determination.These stars are distributed in 35 Kapteyn's Selected Areas, covering thethird and fourth quadrants of the galactic plane (|b| <= 30degr ).The obtained polarization and the known colour excess are compared. Ananalysis of the polarization distribution as a function of the stellardistance is also performed. Based on observations collected at theEuropean Southern Observatory (ESO), La Silla, Chile.
| The Angular Momentum of Main Sequence Stars and Its Relation to Stellar Activity
Rotational velocities are reported for intermediate-mass main sequencestars it the field. The measurements are based on new, high S/N CCDspectra from the Coudé Feed Telescope of the Kitt Peak NationalObservatory. We analyze these rotation rates for a dependence on bothmass and age. We compare the average rotation speeds of the field starswith mean velocities for young stars in Orion, the Alpha Persei cluster,the Pleiades, and the Hyades. The average rotation speeds of stars moremassive than $\sim1.6$ \msun\experience little or no change during theevolutionary lifetimes of these stars on the zero age main sequence orwithin the main sequence band. Less massive stars in the range betwee n1.6\msun\ and 1.3\msun\ also show little decline in mean rotation ratewhile they are on the main sequence, and at most a factor of 2 decreasein velocity as they evolve off the main sequence. The {\it e}-foldingtime for the loss of angular momentum b y the latter group of stars isat least 1--2 billion years. This inferred characteristic time scale forspindown is far longer than the established rotational braking time forsolar-type stars with masses below $\sim1.3$ \msun. We conclude from acomparison of the trends in rotation with trends in chromospheric andcoronal activity that the overall decline in mean rotation speed alongthe main sequence, from $\sim2$ \msun\ down to $\sim1.3$ \msun, isimposed during the pre-main sequence phase of evolution, and that thispattern changes little thereafter while the star resides on the mainsequence. The magnetic activity implicated in the rotational spindown ofthe Sun and of similar stars during their main sequence lifetimes mus ttherefore play only a minor role in determining the rotation rates ofthe intermediate mass stars, either because a solar-like dynamo is weakor absent, or else the geometry of the magnetic field is appreciablyless effective in removing angular momentu m from these stars. (SECTION:Stars)
| Mesures de vitesses radiales. VIII. Accompagnement AU sol DU programme d'observation DU satellite HIPPARCOS
We publish 1879 radial velocities of stars distributed in 105 fields of4^{\circ} \times 4^{\circ}. We continue the PPO series \cite[(Fehrenbachet al. 1987;]{Feh87} \cite[Duflot et al. 1990, 1992 and 1995),]{Du90}using the Fehrenbach objective prism method. Table 1 only available inelectronic form at CDS via to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC).
The positions of 53 FK5, 70 FK5 Extension and 486 GC stars are given forthe equator and equinox J2000.0 and for the mean observation epoch ofeach star. They are determined with the photoelectric astrolabe ofYunnan Observatory. The internal mean errors in right ascension anddeclination are +/- 0.046" and +/- 0.059", respectively. The meanobservation epoch is 1989.51.
| Ca II H and K Filter Photometry on the UVBY System. II. The Catalog of Observations
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....109.2828T&db_key=AST
| Early type high-velocity stars in the solar neighborhood. IV - Four-color and H-beta photometry
Results are presented from photometric obaservations in the Stromgrenuvby four-color and H-beta systems of early-type high-velocity stars inthe solar neighborhood. Several types of photometrically peculiar starsare selected on the basis of their Stromgren indices and areprovisionally identified as peculiar A stars, field horizontal-branchstars, metal-poor stars near the Population II and old-disk turnoffs,metal-poor blue stragglers, or metallic-line A stars. Numerousphotometrically normal stars were also found.
| The early F-type stars - Refined classification, confrontation with Stromgren photometry, and the effects of rotation
The classification for early F-type stars in the MK spectralclassification system presented by Gray and Garrison (1987) is refined.The effect of rotation on spectral classification and ubvy-betaphotometry of early F-type stars is examined. It is found that theclassical luminosity criterion, the 4417 A/4481 A ratio givesinconsistent results. It is shown that most of the stars in the DeltaDelphini class of metallic-line stars are either normal or areindistinguishable from proto-Am stars. It is suggested that thedesignation Delta Delphini should be dropped. The classifications arecompared with Stromgren photometry. The effects of rotation on thedelta-c1 index in the early-F field dwarfs is demonstrated.
| Two-colour diagrams for differentially rotating stars
Not Available
| The Boehm-Vitense gap in the Geneva photometric system
A gap among A-F stars is searched on the main sequence of differentstellar samples in the photometric space M defined by the four colorindexes U-B1, B1-B2, B2-V1 and V1-G of the Geneva photometric system. Agap is noticed for the field and the eight young open clustersinvestigated when selected stars are not visual or spectroscopicbinaries, and not chemically peculiar. It is shown that this gap isinduced by the existence of two differently oriented star branches in M,the so-called radiative and convective branches. The gap is suggestednot to be only a mere artefact of having previously excluded Am and Apstars but partly due to an abrupt onset of convection in late A stars asproposed by Boehm-Vitense (1970). The locus of the gap's red edgeaccording to B2-V1 with regard to the diffusion region, the lowerinstability strip and the low rotational velocities domain supports theidea that the onset of convection lowers the metallicity, stabilizes thepulsations and brakes the rotation. The locus of the gap's blue edgeseems to be connected with age.
| Final catalogue of 229 photometric standards in UBV system near the selected areas 1-115
Not Available
| Photoelectric UVBY and H BET photometry of 750 A and F stars in 63 selected areas with |b|<30
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977A&AS...30..297K&db_key=AST
| Photometric standards on the UBV and RI systems.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975PASP...87..107E&db_key=AST
| Study of the F-type 1 MK spectral types.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975AJ.....80..637M&db_key=AST
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הכנס מאמר חדש
לינקים קשורים
הכנס לינק חדש
משמש של הקבוצה הבאה
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תצפית ומידע אסטרומטרי
| קבוצת-כוכבים: | חד קרן |
| התרוממות ימנית: | 06h48m19.00s |
| סירוב: | -01°19'09.0" |
| גודל גלוי: | 5.75 |
| מרחק: | 40.08 פארסק |
| תנועה נכונה: | -36.7 |
| תנועה נכונה: | -34.2 |
| B-T magnitude: | 6.076 |
| V-T magnitude: | 5.767 |
קטלוגים וכינוים:
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