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The effect of rotation on the abundances of the chemical elements of the A-type stars in the Praesepe cluster
Aims. We study how chemical abundances of late B-, A-, and early F-typestars evolve with time, and we search for correlations between theabundance of chemical elements and other stellar parameters, such aseffective temperature and υ sin i. Methods: We observed a largenumber of B-, A-, and F-type stars belonging to open clusters ofdifferent ages. In this paper we concentrate on the Praesepe cluster(log t = 8.85), for which we have obtained high-resolution, highsignal-to-noise ratio spectra of sixteen normal A- and F-type stars andone Am star, using the SOPHIE spectrograph of the Observatoire deHaute-Provence. For all the observed stars, we derived fundamentalparameters and chemical abundances. In addition, we discuss anothereight Am stars belonging to the same cluster, for which the abundanceanalysis had been presented in a previous paper. Results: We find astrong correlation between the peculiarity of Am stars and υ sin i.The abundance of the elements underabundant in Am stars increases withυ sin i, while it decreases for the overabundant elements. Chemicalabundances of various elements appear correlated with the ironabundance.Based on observations made at the Observatoire de Haute-Provence.Figures [see full textsee full textsee full text] to [see full textseefull textsee full text] are only available in electronic form athttp://www.aanda.org
| Late stages of the evolution of A-type stars on the main sequence: comparison between observed chemical abundances and diffusion models for 8 Am stars of the Praesepe cluster
Aims.We aim to provide observational constraints on diffusion modelsthat predict peculiar chemical abundances in the atmospheres of Amstars. We also intend to check if chemical peculiarities and slowrotation can be explained by the presence of a weak magnetic field. Methods: We have obtained high resolution, high signal-to-noise ratiospectra of eight previously-classified Am stars, two normal A-type starsand one Blue Straggler, considered to be members of the Praesepecluster. For all of these stars we have determined fundamentalparameters and photospheric abundances for a large number of chemicalelements, with a higher precision than was ever obtained before for thiscluster. For seven of these stars we also obtained spectra in circularpolarization and applied the LSD technique to constrain the longitudinalmagnetic field. Results: No magnetic field was detected in any of theanalysed stars. HD 73666, a Blue Straggler previously considered as anAp (Si) star, turns out to have the abundances of a normal A-type star.Am classification is not confirmed for HD 72942. For HD 73709 we havealso calculated synthetic Δ a photometry that is in good agreementwith the observations. There is a generally good agreement betweenabundance predictions of diffusion models and values that we haveobtained for the remaining Am stars. However, the observed Na and Sabundances deviate from the predictions by 0.6 dex and ≥0.25 dexrespectively. Li appears to be overabundant in three stars of oursample.Figures 13-22 and Table 4 are only available in electronic form athttp://www.aanda.org
| Contribution to the search for binaries among Am stars - VIII. New spectroscopic orbits of eight systems and statistical study of a sample of 91 Am stars
This paper is the last of a series devoted to the study of Am stars,with the monitoring of radial velocities of a sample of 91 objectsduring more than 20 yr. The purpose was to determine which stars weremembers of spectroscopic binaries (SBs) and study in detail thosesystems in order to obtain observational constraints on the origin ofthe Am phenomenon.In the first part, we present the results of a detailed study of eightAm stars (HD 32893, 60489, 109762, 111057, 113697, 204918, 219675 andBD+44° 4512) observed at the Haute-Provence and Cambridgeobservatories with CORAVEL instruments. We find that these objects aresingle-lined SBs whose orbital elements are determined for the firsttime. HD 32893 is found to be a triple spectroscopic system whose thirdbody might be detected by speckle interferometry. Physical parametersare inferred for the primaries of those SBs. We then investigate theinfluence of tidal interaction and find that it has already led to thesynchronism of the primaries and to the circularization of the orbits offour of those systems.In the second part of this paper, we present the main results of ourwhole programme and derive some statistical properties of Am stars. Wegive the recapitulating table of the orbital parameters found for theSBs of our whole sample and the list of those for which no evidence forradial velocity variations could be found during our monitoring. Ourstudy shows that at least 64 per cent of Am stars are members of SBs.This rate is significantly greater than that of normal stars. Althoughsome SBs may have been not detected, this study shows that a substantialfraction of Am stars do not belong to SBs: they are either isolatedstars or members of wide binary systems.We then present some statistical properties of the orbital parameters ofthe SBs whose primary is an Am star, on an extended sample obtained byadding 29 Am SB orbits published by other authors. The corresponding eversus logP diagram shows a cut-off between the circular and theeccentric systems at P ~ 5.6 +/- 0.5 d, which indicates a typical age of0.5 - 1 × 109 yr for the Am stars, which is inagreement with the values found in our previous detailed studies. AMonte Carlo analysis shows that the distribution of the mass functionvalues f(m) is compatible with a power-law distribution N(m) ~m-α of the masses m of the companions with α =0.3 +/- 0.2 or with a Gaussian distribution centred on 0.8 +/-0.5Msolar, which indicates that the companions of Am SBs aremostly dwarf stars of type G-K-M.
| AmFm Stars as a Test of Rotational Mixing Models
Stellar evolution models have been calculated for stars of 1.7-2.5Msolar with both the Geneva-Toulouse and Montreal codes. Inthe Geneva-Toulouse code, the internal evolution of angular momentum iscalculated self-consistently along with the transport of a few species.In the Montreal code, the transport of 24 species is treated in detail,taking into account radiative accelerations, thermal diffusion, andgravitational settling, along with the turbulent diffusion coefficientscalculated in the Geneva-Toulouse code. It is verified that the twocodes lead to very similar internal structure for a given mass. Thecalculated surface abundances are compared to abundance anomaliesobserved on AmFm stars. It is found that with approximately the sameparameters as used for other types of stars, the Geneva-Toulouse codeleads to turbulent transport coefficients that produce abundanceanomalies consistent with the observed ones for HD 73045, HD 23610, andSirius. Taking into account the effect of the anisotropy of turbulenceon vertical transport plays an important role, although the level ofanisotropy in stellar envelopes is very uncertain; this effect isusually neglected in calculations. The stabilizing effect of the meanmolecular weight gradient can also be important. The current level ofaccuracy of observed abundances only permits to choose within aone-parameter family of models. To distinguish between turbulent modelswith different interior profiles, an accuracy of 0.03 dex is required ofabundance determinations, a level of accuracy that is not currentlyachieved. It is also shown that taking into account thepre-main-sequence evolution of the rotation profile leads to animportant reduction in the Ω dependence of turbulent transport forslow rotators.
| Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| Zero-Age Main Sequence in the HR Diagram of the Vilnius Photometric System
The zero-age main sequence for solar metallicity stars in the absolutemagnitude vs. color diagram of the Vilnius seven-color photometricsystem is determined. The calibration is based on the results ofphotoelectric photometry of stars in the Hyades, Pleiades and Praesepeopen clusters and the Ori OB1 association. A theoretical Victoria-Reginaisochrone, corresponding to an age of 10 million years, coincides wellwith the lower envelope of the unevolved main sequence.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| SB9: The ninth catalogue of spectroscopic binary orbits
The Ninth Catalogue of Spectroscopic Binary Orbits(http://sb9.astro.ulb.ac.be) continues the series of compilations ofspectroscopic orbits carried out over the past 35 years by Batten andcollaborators. As of 2004 May 1st, the new Catalogue holds orbits for2386 systems. Some essential differences between this catalogue and itspredecessors are outlined and three straightforward applications arepresented: (1) completeness assessment: period distribution of SB1s andSB2s; (2) shortest periods across the H-R diagram; (3)period-eccentricity relation.
| Abundance analysis of Am binaries and search for tidally driven abundance anomalies - I. HD 33254, HD 178449 and HD 198391
It is suggested that if the tidally induced meridional circulation ofTassoul & Tassoul existed, it might successfully compete withdiffusion processes and rotationally induced meridional circulation.This could affect the chemical composition of an Am binary component.The main goal of this paper is to start a systematic abundance analysisof a sample of Am binaries in order to search for possible observableabundance anomalies driven by tidal interaction in these binary systems.A synthetic spectrum analysis of CCD observations in two spectralregions (6400-6500 and 6660-6760 Å) of HD 33254, HD 178449 and HD198391 was carried out. Basic stellar properties, atmospheric parametersand abundance patterns were derived. HD 33254 is the star withpronounced Am anomalies, while HD 198391 is found to be an extremelysharp-lined hot Am star. HD 178449 is a controversial and extremelyhighly rotating star. We have succeeded in detecting a very faintsecondary spectrum. The most probable explanation is that we havediscovered the new spectroscopic Ab component of this spectroscopic andvisual multiple system.
| Astrometric radial velocities. III. Hipparcos measurements of nearby star clusters and associations
Radial motions of stars in nearby moving clusters are determined fromaccurate proper motions and trigonometric parallaxes, without any use ofspectroscopy. Assuming that cluster members share the same velocityvector (apart from a random dispersion), we apply a maximum-likelihoodmethod on astrometric data from Hipparcos to compute radial and spacevelocities (and their dispersions) in the Ursa Major, Hyades, ComaBerenices, Pleiades, and Praesepe clusters, and for theScorpius-Centaurus, alpha Persei, and ``HIP 98321'' associations. Theradial motion of the Hyades cluster is determined to within 0.4 kms-1 (standard error), and that of its individual stars towithin 0.6 km s-1. For other clusters, Hipparcos data yieldastrometric radial velocities with typical accuracies of a few kms-1. A comparison of these astrometric values withspectroscopic radial velocities in the literature shows a good generalagreement and, in the case of the best-determined Hyades cluster, alsopermits searches for subtle astrophysical differences, such as evidencefor enhanced convective blueshifts of F-dwarf spectra, and decreasedgravitational redshifts in giants. Similar comparisons for the ScorpiusOB2 complex indicate some expansion of its associations, albeit slowerthan expected from their ages. As a by-product from the radial-velocitysolutions, kinematically improved parallaxes for individual stars areobtained, enabling Hertzsprung-Russell diagrams with unprecedentedaccuracy in luminosity. For the Hyades (parallax accuracy 0.3 mas), itsmain sequence resembles a thin line, possibly with wiggles in it.Although this main sequence has underpopulated regions at certaincolours (previously suggested to be ``Böhm-Vitense gaps''), suchare not visible for other clusters, and are probably spurious. Futurespace astrometry missions carry a great potential for absoluteradial-velocity determinations, insensitive to the complexities ofstellar spectra. Based on observations by the ESA Hipparcos satellite.Extended versions of Tables \ref{tab1} and \ref{tab2} are available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.125.8) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/381/446
| Binarity of Am stars in Praesepe and Hyades
CORAVEL radial-velocity observations of Am stars in the Hyades andPraesepe have allowed the determination of orbital elements for 10spectroscopic binaries, among which 3 are first determinations. One Amstar (KW 40) is found to be a well hierarchisedtriple system. KW 538 has a rather long period (435days) for an Am star. Orbits of systems with periods shorter than 8.5days are circularized, or present eccentricities smaller than 0.04. For19 Am stars, the number of quadruple-, triple-, double-, single systemsis 1:2:14(10+4?):(2?). The Am stars in a (beta , B-V) diagram clearlystand away by 0.03 mag from the sequence defined by normal main-sequencestars. This diagram could be a powerful method to identify Am stars inmore distant open clusters, provided there is no differential reddening.In the colour-magnitude diagram (M_V, beta ), double-lined binaries are0.6 - 0.7 mag above the ZAMS as expected, while most single-lined areclose to or on the ZAMS because the secondary does not contribute muchlight. The absence of X-ray detection of 4 systems in the Hyades is anargument for the presence of a white dwarf secondary. based onobservations collected at the Haute-Provence Observatory(France)}\fnmsep \thanks{Table~2 is available only in electronic form atCDS by ftp at 130.79.128.5 or on the Web athttp://cdsweb.u-strasbg.fr/CDS.html
| The Pleiades, Coma, Hyades, and Praesepe open clusters: Li, Al, Si, S, Fe, Ni, and Eu abundances compared in A stars
In the third of a series of papers on the A stars in open clusters, theComa and Hyades clusters are revisited; in the first and second papers,the Pleiades and Praesepe were respectively investigated. All thespectra were secured with the Canada-France-Hawaii telescope at highspectral resolution and high signal-to-noise ratios. Photosphericabundances have been determined for Li, Al, Si, S, Fe, Ni, and Eu frommodel atmosphere abundance analysis. All the A stars with enough-sharplines to be studied for Li were observed in the four clusters. Abundanceresults are summarized for 31 cluster members, including 21 Am, 7 normalA, and 3 early-A stars. The Am stars have very uniform Li, Al, Si, S,and Fe abundances in a large temperature range of nearly 1000 K.Compared to normal A stars, Li is significantly deficient in Am stars(by a factor of 3), Al marginally overabundant, Si, S, and Fe are thesame, Ni and Eu (with only a few results) overabundant. Those uniformabundances of Li, Al, Si, S, or Fe in Am stars involve that abundancesare little affected by the magnitude of the rotational velocity. Forboth Am and normal A samples, no abundance trend as a function of ageand/or evolution is detected in the case of Li, Al, Si, S, or Fe. Theages considered are in the range 0.8 - 7 108 years; theevolution is limited from the ZAMS to the cluster turn-off. The build-upof the chemical abundances studied, in particular the Li differentiationbetween Am and normal A stars, could have taken place very early whenthe stars arrive on the Main Sequence. The spread in lithium found forthe A stars is reminiscent of that reported in the field and one opencluster for stars of nearly the same mass and slightly evolved out ofthe Main Sequence. The Li abundance does not change as soon as the starevolves through the subgiant phase and the convection zone becomesdeeper. There are two exceptional Am stars: one, in the Hyades, isLi-deficient and the other, in Praesepe, Li-overabundant. They are noobvious circumstances that can distinguish both stars from others in thevery same region of their respective cluster sequence. In each of thefour clusters, the maximum Li abundance is found in A stars, generallyin normal A stars. The Fe abundance of both Am and normal A groups isfound to be twice the original Fe value (on the ZAMS) in each of thefour clusters, independently of their age or metallicity. It is wellestablished for the Am group and in only a narrow range of Teff for thenormal A group. This behavior is unexpected for normal A stars which arethought to have their original abundances and Fe abundance differentfrom that of Am stars. A larger normal A sample is needed to concludeanything. Our abundance results for cluster Am stars quantitativelyagree with predictions of new models coupling atomic diffusion withturbulent transport (Richer et al. \cite{richer99}). Based onobservations collected at the Canada-France-Hawaii telescope (Hawaii)
| The Evolution of AMFM Stars, Abundance Anomalies, and Turbulent Transport
Stellar evolution models of stars of 1.45-3.0 Msolar havebeen calculated, including the atomic diffusion of metals and radiativeaccelerations for all species in the OPAL opacities. As the abundanceschange, the opacities and radiative accelerations are continuouslyrecalculated during evolution. These models develop iron-peak convectionzones centered at a temperature of approximately 200,000 K. If one thenassumes that there is sufficient overshoot to homogenize the surfaceregions between the hydrogen, helium, and iron-peak convection zones, itis shown here that the surface abundance variations that are produced,without any arbitrary parameter, closely resemble the abundanceanomalies of AmFm stars, except that they are larger by a factor ofabout 3. Detailed evolutionary model calculations have been carried out,varying the turbulence in the outer stellar regions in order to improvethe agreement with the observed anomalies in AmFm stars. The outer massmixed by turbulence has been varied, as well as the density dependenceof the turbulent diffusion coefficient. It is shown that the anomaliesdepend on only one parameter characterizing turbulence, namely, thedepth of the zone mixed by turbulence. The calculated surface abundancesare compared to observations of a number of recently observed AmFmstars. For Sirius A, 16 abundances (including four upper limits) areavailable for comparison. Of these, 12 are well reproduced by the model,while three are not so well reproduced, and one is a very uncertainobservation. In cluster AmFm stars, the age and initial abundances areknown. There is then less arbitrariness in the calculations, but fewerchemical species have been observed than in Sirius. The availableobservations (Hyades, Pleiades, and Praesepe stars are compared) agreereasonably well with the calculated models for the five stars that arecompared. The zone mixed by turbulence is deeper than the ironconvection zone, reducing the abundance anomalies to values that are toosmall for iron-peak convection zones to develop in many of the models.The origin of the mixing process then remains uncertain. There isconsiderable scatter in the observations between different observers, soit is premature to conclude that hydrodynamical processes other thanturbulence are needed to explain the observations. We do not rule outthe possibility that this might be the case, but the observations do notappear to us to be good enough to establish it.
| Open clusters with Hipparcos. I. Mean astrometric parameters
New memberships, mean parallaxes and proper motions of all 9 openclusters closer than 300 pc (except the Hyades) and 9rich clusters between 300 and 500 pc have been computed using Hipparcosdata. Precisions, ranging from 0.2 to 0.5 mas for parallaxes and 0.1 to0.5 mas/yr for proper motions, are of great interest for calibratingphotometric parallaxes as well as for kinematical studies. Carefulinvestigations of possible biases have been performed and no evidence ofsignificant systematic errors on the mean cluster parallaxes has beenfound. The distances and proper motions of 32 more distant clusters,which may be used statistically, are also indicated. Based onobservations made with the ESA Hipparcos astrometry satellite
| The Praesepe open cluster: abundances of Li, Al, Si, S, Fe, Ni, and EU in A stars.
In the second of a series of papers on the A stars in open clusters, thePraesepe cluster is investigated; in the first paper, it was thePleiades. Ten A Praesepe stars were observed with theCanada-France-Hawaii telescope at high spectral resolution and highsignal-to-noise ratios. Photospheric abundances of the sample, which hasturned out to be composed exclusively with Am stars, have beendetermined for Li, Al, Si, S, Fe, Ni, and Eu from model atmosphereabundance analysis. The A stars of Praesepe are well advanced in theMain Sequence evolution: several of the observed stars are in theturn-off (and one is a blue straggler). The Li abundance in Am stars isthe same as in non-evolved Praesepe F stars on the hot side of the Lidip, and Fe is twice its original value as given by Praesepe F stars.The abundances of the studied elements were found remarkably uniform inthe cluster over a large range of T_eff, i.e., for various structureenvelopes and evolution. Surface abundances of Li and Fe remainunchanged in Am stars at both ages of the Pleiades and Praesepeclusters. The Li results for the Am stars challenge predictions fromevolutionary model envelopes in the framework of a diffusion-dominantdescription. Based on observations collected at the Canada-France-Hawaiitelescope (Hawaii)
| Evolution of mass segregation in open clusters: some observational evidences
On the basis of the best available member list and duplicityinformation, we have studied the radial structure of Praesepe and of thevery young open cluster NGC 6231. We have found mass segregation amongthe cluster members and between binaries and single stars, which isexplained by the greater average mass of the multiple systems. However,the degree of mass segregation for stars between 1.5 and 2.3 M_sun isless pronounced in Praesepe than in the Pleiades. Furthermore, masssegregation is already present in the very young open cluster NGC 6231although this cluster is likely still not dynamically relaxed. Wediscuss the implications of these results and propose a qualitativescenario for the evolution of mass segregation in open clusters. InPraesepe the mass function of single stars and primaries appears to besignificantly different, like in the Pleiades. We observe an absence ofellipticity of the outer part of Praesepe. Tables 2 and 3 are availableonly in electronic form from the Strasbourg ftp server at 130.79.128.5
| Metal abundances of A-type stars in three galactic clusters.
Investigations have been carried out for 11 A stars in young openclusters (α Per, Coma, and Praesepe) and three field stars bymeans of high resolution spectroscopy. Detailed abundance analyses havebeen made for Mg, Ca, Sc, Cr, Fe, and Ni. The results are discussed inthe framework of element stratification processes as invoked bytime-dependent diffusion mechanisms in Am stars. The youngest cluster ofour sample, α Per, seems to show some untypical abundance patternswhich might be identified as early Am phases.
| 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.
| ICCD speckle observations of binary stars. IX - A duplicity survey of the Pleiades, Praesepe, and IC 4665 clusters
Multiplicity of stars within clusters is a well-studied phenomenon.However, recent survey work done on the Hyades by Mason et al. (1993)would seem to indicate that even in the most often studied clusters,there may be binaries yet undiscovered. In order to expand the sample ofcluster binaries with potentially short-period visual orbits, a specklesurvey of 45 Pleiades, 54 Praesepe, and 22 IC 4665 bright stars (V isless than 10) for possible multiplicity was conducted at the KPNO 4 mMayall telescope between 1987 October and 1991 November. Of these, threenew binaries have been discovered: one in the Pleiades where the newcomponent may be spectroscopic, another in Praesepe which has beenconfirmed from examinations of archival observations and also has beenresolved by occultation, and the third in IC 4665. Continued study ofthese new binary stars could further refine the cluster distance modulias well as the cluster mass-luminosity relations.
| Liste des étoiles Ap et Am dans les amas ouverts (édition révisée)
Not Available
| Photometric binary stars in Praesepe and the search for globular cluster binaries
A radial velocity study of the stars which are located on a secondsequence above the single-star zero-age main sequence at a given colorin the color-magnitude diagram of the open cluster Praesepe, (NGC 2632)shows that 10, and possibly 11, of 17 are binary systems. Of the binarysystems, five have full amplitudes for their velocity variations thatare greater than 50 km/s. To the extent that they can be applied toglobular clusters, these results suggests that (1) observations of'second-sequence' stars in globular clusters would be an efficient wayof finding main-sequence binary systems in globulars, and (2) currentinstrumentation on large telescopes is sufficient for establishingunambiguously the existence of main-sequence binary systems in nearbyglobular clusters.
| Liste des étoiles Ap et Am dans les amas ouverts (Edition révisée)
Not Available
| Investigation of the Praesepe cluster. I - Identification of halo members
Coravel radial velocities and UBVRI (Kron) photometry of 117 starsselected by their proper motion in the region surrounding Praesepe (NGC2632, C 0837 + 201) have permitted identification of 48 members of thecluster halo, up to a distance of 4 deg from the cluster center. The 43(F5-K0) new members represent 51 percent of the number of nucleusmembers known in this spectral interval. Ten spectroscopic binaries havebeen discovered among the F5-F0 members, resulting in a frequency of 23percent, which rises to 33 percent four probable binaries are taken intoaccount. Six orbits have been obtained, with periods ranging from 1.2 to143 d. Four additional binaries have been detected among the non-memberstars.
| Catalog of AP and AM stars in open clusters
The previous results of Raab (1922), Markarian (1951), and Collinder(1931) have been used to catalog Ap and Am stars that are in the fieldof open clusters. Tabular data are presented for the clusterdesignation, the HD or HDE number, the right ascension (1900), thedeclination (1900), and the magnitude. Also listed are the spectraltypes and, for certain stars, the probability of cluster membership.
| Chemically peculiar stars in open clusters. I - The catalog
The largest existing compilation is presented of Ap and Am open clusterstars. The catalog contains information on 381 chemically peculiar (CP)stars of the upper main sequence in 79 open clusters. The catalog iscomposed of the following tables: (1) the main body, which lists CP (orsuspected CP) stars which are kinematical (or suspected kinematical)members of open clusters; (2) the list of CP (or suspected CP) starssometimes numbered among cluster members but which are actuallykinematical nonmembers; (3) the list of stars sometimes designated as'peculiar' but, in fact, probably not CP; (4) references for numberingsystems of cluster stars; (5) references for membership; and (6)references for spectral and/or peculiarity types.
| MK classification of the brighter praesepe stars
MK classifications have been obtained for the 42 brightest stars in therich open cluster Praesepe. In the H-R diagram, 10 of the 12 starsbrighter than V = 7.0 mag have luminosity classes brighter than V or areAm stars. Only two of the stars fainter than V = 7.0 mag are ofluminosity class IV. The nine Am stars discovered by Bidelman (1956) areconfirmed. The frequency of these among the late A stars is consistentwith results for field stars, but there is only one Ap star. The reasonsfor that deficiency are discussed.
| A Proper Motion Membership Study of Praesepe
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983AJ.....88..215J&db_key=AST
| 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
| The rotational velocity effect on the main sequence AM stars metallicity
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1979A&A....74...38B&db_key=AST
| Spectral classification of stars with the same colours in intermediate multiband photometry - The concept of photometric 'star-box'
The concept of a photometric 'star box' is introduced for use with the UB V B1 B2 V1 G photometric system. Star boxes are employed to grouptogether all stars for which each photometric color differs by less thansome small quantity (in magnitude) from the corresponding color of agiven 'central' star. Probable causes of differences between the colorsof two stars are summarized, scatter in spectral type and luminosityclass within a single box is discussed, and the standard deviation ofnarrow-band photometric indices is calculated for stars grouped in thesame box. Dispersions in the UV and IR energy distributions of stars inthe same box are examined, and the results obtained in the seven-colorphotometric system for 113 stars are compared with the correspondingresults in a thirteen-color system. The classification of Am and Am:stars is briefly examined on the basis of star boxes.
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Pozíciós és asztrometriai adatok
| Csillagkép: | Rák |
| Rektaszcenzió: | 08h36m48.00s |
| Deklináció: | +18°52'58.1" |
| Vizuális fényesség: | 8.622 |
| Távolság: | 201.207 parszek |
| RA sajátmozgás: | -36 |
| Dec sajátmozgás: | -13.1 |
| B-T magnitude: | 8.987 |
| V-T magnitude: | 8.653 |
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