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Analysing the Hipparcos epoch photometry of λ Bootis stars
We performed a homogeneous analysis of the available Hipparcos epochphotometry for all members of the LB group. Besides the known δScuti like pulsation frequencies, we searched for eclipses due tobinarity or rotational induced variability. The already knownfrequencies of HD 15165 are confirmed with an additional lower singlefrequency, which might be caused by an accretion episode. But we are notable to rule out a possible aliasing due to the temporal sampling of thedata set. Furthermore, three candidates (HD 15759, HD 120500, and HD149130) for a possible eclipse were detected. Otherwise, the frequencyanalysis reveals a null result within our strict detection limits.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| The heterogeneous class of lambda Bootis stars
We demonstrate that it is arduous to define the lambda Boo stars as aclass of objects exhibiting uniform abundance peculiarities which wouldbe generated by a mechanism altering the structure of their atmosphericlayers. We collected the stars classified as lambda Boo up to now anddiscuss their properties, in particular the important percentage ofconfirmed binaries producing composite spectra (including our adaptiveoptics observations) and of misclassified objects. The unexplained RVvariables (and thus suspected binaries), the known SB for which we lackinformation on the companion, the stars with an UV flux inconsistentwith their classification, and the fast rotating stars for which noaccurate abundance analysis can be performed, are also reviewed.Partly based on observations collected at the CFH Telescope (Hawaii) andat TBL of the Pic du Midi Observatory (France).Table \ref{tab5} is only available in electronic form athttp://www.edpsciences.org
| The elemental abundance pattern of twenty lambda Bootis candidate stars
Detailed elemental abundances were derived for twenty bona fide lambdaBootis as well as two MK standard stars. Other than LTE abundances forten elements (including C and O), NLTE values for Na were determined.The group of lambda Bootis stars consists of non-magnetic, Population I,late B to early F-type dwarfs with a typical abundance pattern (Fe-peakelements being underabundant whereas C, N, O and S being almost solarabundant). Since classification resolution spectroscopy in the opticaldomain is not capable of determining the abundance of the lightelements, a detailed abundance analysis is the ultimate test for themembership of an object to this group. Another important point is thedetection of apparent spectroscopic binary systems in which two solarabundance objects mimic one metal-weak star, as proposed as a workinghypothesis by Faraggiana & Bonifacio (\cite{farag99}). From twentyprogram stars we are able to confirm or establish the membership fornine objects (HD 23258, HD 36726, HD 40588, HD 74911, HD 84123, HD91130, HD 106223, HD 111604 and HD 290799). Five stars (HD 90821, HD98772, HD 103483, HD 108765 and HD 261904) can be definitely ruled outas being members of the lambda Bootis group whereas no unambiguousdecision can be drawn for another six stars (HD 66684, HD 105058, HD120500, HD 141851, HD 201184 and HD 294253). One very important resultis the apparent overabundances found for Na which cannot be explained byaccretion or mass-loss alone. Based on observations from theOsservatorio Astronomico di Padova-Asiago, McDonald Observatory, KittPeak National Observatory and Observatório do Pico dosDias-LNA/CNPq/MCT.
| 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.
| On the Period-Luminosity-Colour-Metallicity relation and the pulsational characteristics of lambda Bootis type stars
Generally, chemical peculiarity found for stars on the upper mainsequence excludes delta Scuti type pulsation (e.g. Ap and Am stars), butfor the group of lambda Bootis stars it is just the opposite. This makesthem very interesting for asteroseismological investigations. The groupof lambda Bootis type stars comprises late B- to early F-type,Population I objects which are basically metal weak, in particular theFe group elements, but with the clear exception of C, N, O and S. Thepresent work is a continuation of the studies by Paunzen et al.(\cite{Pau97}, \cite{Pau98}), who presented first results on thepulsational characteristics of the lambda Bootis stars. Since then, wehave observed 22 additional objects; we found eight new pulsators andconfirmed another one. Furthermore, new spectroscopic data (Paunzen\cite{Pau01}) allowed us to sort out misidentified candidates and to addtrue members to the group. From 67 members of this group, only two arenot photometrically investigated yet which makes our analysis highlyrepresentative. We have compared our results on the pulsationalbehaviour of the lambda Bootis stars with those of a sample of deltaScuti type objects. We find that at least 70% of all lambda Bootis typestars inside the classical instability strip pulsate, and they do sowith high overtone modes (Q < 0.020 d). Only a few stars, if any,pulsate in the fundamental mode. Our photometric results are inexcellent agreement with the spectroscopic work on high-degree nonradialpulsations by Bohlender et al. (\cite{Boh99}). Compared to the deltaScuti stars, the cool and hot borders of the instability strip of thelambda Bootis stars are shifted by about 25 mmag, towards smaller(b-y)_0. Using published abundances and the metallicity sensitiveindices of the Geneva 7-colour and Strömgren uvbybeta systems, wehave derived [Z] values which describe the surface abundance of theheavier elements for the group members. We find that thePeriod-Luminosity-Colour relation for the group of lambda Bootis starsis within the errors identical with that of the normal delta Scutistars. No clear evidence for a statistically significant metallicityterm was detected. Based on observations from the Austrian AutomaticPhotoelectric Telescope (Fairborn Observatory), SAAO and Siding SpringObservatory.
| Distances and Metallicities of High- and Intermediate-Velocity Clouds
A table is presented that summarizes published absorption linemeasurements for the high- and intermediate-velocity clouds (HVCs andIVCs). New values are derived for N(H I) in the direction of observedprobes, in order to arrive at reliable abundances and abundance limits(the H I data are described in Paper II). Distances to stellar probesare revisited and calculated consistently, in order to derive distancebrackets or limits for many of the clouds, taking care to properlyinterpret nondetections. The main conclusions are the following. (1)Absolute abundances have been measured using lines of S II, N I, and OI, with the following resulting values: ~0.1 solar for one HVC (complexC), ~0.3 solar for the Magellanic Stream, ~0.5 solar for a southern IVC,and ~solar for two northern IVCs (the IV Arch and LLIV Arch). Finally,approximate values in the range 0.5-2 solar are found for three moreIVCs. (2) Depletion patterns in IVCs are like those in warm disk or halogas. (3) Most distance limits are based on strong UV lines of C II, SiII, and Mg II, a few on Ca II. Distance limits for major HVCs aregreater than 5 kpc, while distance brackets for several IVCs are in therange 0.5-2 kpc. (4) Mass limits for major IVCs are0.5-8×105 Msolar, but for major HVCs theyare more than 106 Msolar. (5) The Ca II/H I ratiovaries by up to a factor 2-5 within a single cloud, somewhat morebetween clouds. (6) The Na I/H I ratio varies by a factor of more than10 within a cloud, and even more between clouds. Thus, Ca II can beuseful for determining both lower and upper distance limits, but Na Ionly yields upper limits.
| A spectroscopic survey for lambda Bootis stars. III. Final results
In the third paper of a series dedicated to the spectroscopic survey fornew lambda Bootis stars, we present all new and confirmed members of thegroup as well as a detailed analysis of the observed sample. The natureof this small group of chemically peculiar stars of the upper mainsequence still challenges our understanding of processes like diffusion,mass-loss and accretion. The typical abundances pattern (nearly solarvalues for C, N, O and S whereas the Fe-peak elements are moderate tostrong underabundant) can still not be explained by any proposed theory.Hence, the significant increase of new members gives the opportunity toinvestigate the group properties in more detail. We report the discoveryof 26 new members of the group and the confirmation of 18 candidatesfrom the literature. This almost triples the number of known lambdaBootis stars. The existence of one member in the young open cluster NGC2264 and four members in the Orion OB1 association proves that thelambda Bootis phenomenon already works at very early stages of stellarevolution. Recent results from the Hipparcos mission have shown that thewell established lambda Bootis stars of the Galactic field comprise thewhole area from the Zero Age Main Sequence to the Terminal Age MainSequence (~ 109 yr for an A-type star). There is a continuoustransition between very young and rather evolved evolutionary stages. Wefind that the overall percentage of lambda Bootis type among all normaltype stars in the spectral range from B8 to F4 is 2% in the Galacticfield as well as in open clusters. Furthermore, 44 metal-weak objectsare listed which might be connected with the lambda Bootis phenomenon.Our biased sample (chosen by photometric boxes) is not distinguishedfrom all A-type stars in the corresponding spectral region by therotational velocity distribution. Only for the luminosity classes IV andIII (especially for the cooler program stars) the determined mean v sini values are very high compared to those of the literature. Based onobservations from the Observatoire de Haute-Provence, OsservatorioAstronomico di Padova-Asiago, Observatório do Pico dosDias-LNA/CNPq/MCT, Chews Ridge Observatory (MIRA) and University ofToronto Southern Observatory (Las Campanas).
| A spectroscopic survey for lambda Bootis stars. II. The observational data
lambda Bootis stars comprise only a small number of all A-type stars andare characterized as nonmagnetic, Population i, late B to early F-typedwarfs which show significant underabundances of metals whereas thelight elements (C, N, O and S) are almost normal abundant compared tothe Sun. In the second paper on a spectroscopic survey for lambda Bootisstars, we present the spectral classifications of all program starsobserved. These stars were selected on the basis of their Strömgrenuvbybeta colors as lambda Bootis candidates. In total, 708 objects insix open clusters, the Orion OB1 association and the Galactic field wereclassified. In addition, 9 serendipity non-candidates in the vicinity ofour program stars as well as 15 Guide Star Catalogue stars were observedresulting in a total of 732 classified stars. The 15 objects from theGuide Star Catalogue are part of a program for the classification ofapparent variable stars from the Fine Guidance Sensors of the HubbleSpace Telescope. A grid of 105 MK standard as well as ``pathological''stars guarantees a precise classification. A comparison of our spectralclassification with the extensive work of Abt & Morrell(\cite{Abt95}) shows no significant differences. The derived types are0.23 +/- 0.09 (rms error per measurement) subclasses later and 0.30 +/-0.08 luminosity classes more luminous than those of Abt & Morrell(\cite{Abt95}) based on a sample of 160 objects in common. The estimatederrors of the means are +/- 0.1 subclasses. The characteristics of oursample are discussed in respect to the distribution on the sky, apparentvisual magnitudes and Strömgren uvbybeta colors. Based onobservations from the Observatoire de Haute-Provence, OsservatorioAstronomico di Padova-Asiago, Observatório do Pico dosDias-LNA/CNPq/MCT, Chews Ridge Observatory (MIRA) and University ofToronto Southern Observatory (Las Campanas).
| A speckle interferometry survey of lambda Bootis stars
A search for duplicity of lambda Boo stars has been made by using thespeckle camera installed at the Telescopio Nazionale Galileo. Theoperation mode and the reduction procedure allow one to obtain not onlythe separation, but also the magnitude difference between thecomponents; the latter parameter is fundamental for determining thedegree of contamination from the secondary component of a binary systemand thus the importance of the veiling effect that produces absorptionlines weaker than normal. Two stars, HD 38545 and HD 290492, are closebinaries with values of the separation and of the magnitude differencesuch that only a composite spectrum can be observed. For another 15lambda Boo candidates, observed with negative results, the upper limitsof a possible companion separation are given. Based on observations madewith the Italian Telescopio Nazionale Galileo (TNG) operated on theisland of La Palma by the Centro Galileo Galilei of the CNAA (ConsorzioNazionale per l'Astronomia e l'Astrofisica) at the Spanish Observatoriodel Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
| delta Scuti and related stars: Analysis of the R00 Catalogue
We present a comprehensive analysis of the properties of the pulsatingdelta Scuti and related variables based mainly on the content of therecently published catalogue by Rodríguez et al.(\cite{retal00a}, hereafter R00). In particular, the primaryobservational properties such as visual amplitude, period and visualmagnitude and the contributions from the Hipparcos, OGLE and MACHOlong-term monitoring projects are examined. The membership of thesevariables in open clusters and multiple systems is also analyzed, withspecial attention given to the delta Scuti pulsators situated ineclipsing binary systems. The location of the delta Scuti variables inthe H-R diagram is discussed on the basis of HIPPARCOS parallaxes anduvbybeta photometry. New borders of the classical instability arepresented. In particular, the properties of the delta Scuti pulsatorswith nonsolar surface abundances (SX Phe, lambda Boo, rho Pup, delta Deland classical Am stars subgroups) are examined. The Hipparcos parallaxesshow that the available photometric uvbybeta absolute magnitudecalibrations by Crawford can be applied correctly to delta Scutivariables rotating faster than v sin i ~ 100 km s{-1} withnormal spectra. It is shown that systematic deviations exist for thephotometrically determined absolute magnitudes, which correlate with vsin i and delta m1. The photometric calibrations are found tofit the lambda Boo stars, but should not be used for the group ofevolved metallic-line A stars. The related gamma Dor variables and thepre-main-sequence delta Scuti variables are also discussed. Finally, thevariables catalogued with periods longer than 0fd 25 are examined on astar-by-star basis in order to assign them to the proper delta Scuti, RRLyrae or gamma Dor class. A search for massive, long-period delta Scutistars similar to the triple-mode variable AC And is also carried out.
| 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
| How many lambda Bootis stars are binaries?
In the attempt to shed new light on the lambda Boo phenomenon weanalyzed the astrometric, photometric and spectroscopic characteristicsof stars out of a list of recently selected lambda Boo candidates. Weshow that the class is still ill-defined and discuss the possibilitythat some, if not most stars presently classified as lambda Boo, are infact binary pairs and that peculiar abundances may not correspond toactual values if the average values of the atmospheric parameters{Teff} and log g are assumed and the effect of veiling is nottaken into account. Partly based on data from the ESA Hipparcosastrometry satellite.
| Identification of lambda Bootis stars using IUE spectra. II. High resolution data
Stars included in the catalogue of lambda Bootis stars by Paunzen et al.(\cite{Paunzen97}) with high resolution spectra (FWHM: 0.10-0.25 Ä)in the INES Archive of the International Ultraviolet Explorer satellite(IUE) are analyzed here in order to establish membership criteria forthe lambda Bootis group. Line-ratios of carbon to heavier elements (Si,Al, Ca) were adopted as criteria in the SWP range (1150-1980 Ä).For the LWP range (1850-3350 Ä), the intensity of metallic lines(Fe and Mg) was used. These criteria, together with those derived forlow resolution spectra, make the IUE Final Archive a powerful tool tofind new {lambda Bootis} candidates.
| Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS
Radial velocities have been determined for a sample of 2930 B2-F5 stars,95% observed by the Hipparcos satellite in the north hemisphere and 80%without reliable radial velocity up to now. Observations were obtainedat the Observatoire de Haute Provence with a dispersion of 80Ä,mm(-1) with the aim of studying stellar and galactic dynamics.Radial velocities have been measured by correlation with templates ofthe same spectral class. The mean obtained precision is 3.0 km s(-1)with three observations. A new MK spectral classification is estimatedfor all stars. Based on observations made at the Haute ProvenceObservatory, France and on data from The Hipparcos Catalogue, ESA.Tables 4, 5 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr or viahttp://cdsweb.u-strasbg.fr/Abstract.htm
| Pulsation in lambda Bootis stars
In this paper we present a further step in applying asteroseismictechniques to the group of lambda Bootis stars which can becharacterized as nonmagnetic A to F-type Population I dwarfs withsignificant (surface) underabundances of Fe-peak elements. Since noconclusive theory explaining the origin of the observed abundanceanomalies exists, an extensive photometric survey for pulsation in thisgroup has been initiated. Knowledge about the pulsational properties(most members are located within the classical instability strip) couldhelp to establish constrains about the overall abundance of these starsas well as on the evolutionary status. New photometric observations werecarried out for eleven stars. Variability was detected in four stars(e.g. lambda Bootis itself) whereas the remaining seven objects areprobably constant. In total, 52 members of this group have beenphotometrically investigated so far. With 22 pulsating and 30``constant'' stars, we derive a ratio of at least 50 % for variable tononvariable members inside the classical instability strip. This resultis based on high quality Hipparcos and new photometric data. Theobserved log /lineρ//lineρ_ȯ and log P values for thepulsating members are compatible with standard (solar abundant) deltaScuti models supporting the hypothesis that the found abundanceanomalies are restricted to the surface only. Otherwise the pulsationalproperties of this group are not outstanding compared to ``normal''delta Scuti stars, indicating that the mechanism driving the pulsationsis very similar. Based on observations obtained at ESO-La\,Silla, CTIO,SAAO, McDonald Observatory, Instituto Astrofisica Andalucia Observatoryand with the Hipparcos satellite
| Shell signs in the hydrogen-line spectrum of some lambda Bootis-type stars
The hydrogen-line spectrum of eight lambda Bootis type stars is studied.The observed H delta and H gamma profiles are compared with Kurucz'stheoretical profiles. The existence of weak emission-like details in thecores of five lambda Boo stars is demonstrated. The Inglis-Tellerformula is used to calculate the electron densities. It is found thatelectron densities in the atmospheres of stars with peculiar H-lineprofiles are twice lower than in stars with normal profiles. Theconclusion is made that stars with peculiar profiles exhibit some of thecharacteristics usually observed in stars with extended atmospheres.
| Identification of lambda Bootis stars using IUE spectra. I. Low resolution data
An analysis of the stars included in the catalogue of lambda Bootisstars by Paunzen et al. (1997) and which also have IUE observations ispresented here. Population I A-F type stars as well as field horizontalbranch stars were also included in the analysis. Using line-ratios ofcarbon to heavier elements (Al and Ni) allows us to establishunambiguous membership criteria for the lambda Bootis group. Tables 1-3are only available in electronic form at CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| A spectroscopic survey for lambda Bootis stars. I. Strategy, techniques and first results
In recent years, the chemically peculiar (CP) stars of the upper mainsequence have become a fruitful field for the testing of astrophysicaltheories. Processes such as diffusion, convection and mass loss havebeen developed theoretically and introduced into models. The group oflambda Bootis stars, however, is remarkable among the chemicallypeculiar stars as they are nonmagnetic, Population I, A to F-type dwarfswhich show significant underabundances of metals (except for C, N, O andS). Unfortunately, the small number of confirmed members of the lambdaBootis class makes a sound statistical analysis of their propertiesimpossible. Thus, it is still difficult to decide between the twotheories - mass loss with diffusion and the accretion theory - whichhave been proposed to explain the origin of these stars. We thereforehave started a spectroscopic survey to find new lambda Bootis stars inthe field as well as in open clusters and associations. The presence oflambda Bootis stars in open clusters and associations would permit adetermination of the ages of these stars, and thus would yield animportant test for distinguishing between the two theories. In thispaper we describe the selection of candidates using photometriccriteria, the basic requirements, spectroscopic follow-up observationsand results from the first three observing runs. Special care was takento avoid misclassification of our programme stars (e.g. lambda Bootisstars are often confused with intermediate Population II, He-weak orhigh v sin i stars), using a refined MK system. The discovery of atleast six new lambda Bootis stars (including three in the Orion OB1association) shows the efficacy of our selection criteria. Based onobservations obtained at the Observatoire de Haute-Provence and the DarkSky Observatory.
| On the evolutionary status of λ Bootis stars using HIPPARCOS data.
We have used the Hipparcos data to derive absolute magnitudes and thusthe evolutionary status for the group of λ Bootis stars. Theorigin for this small group of nonmagnetic, chemically peculiar stars,still remains a matter of debate. Using new evolutionary tracks, we areable to provide an age determination to distinguish between the twoproposed theories - the diffusion/mass-loss and the accretion theory.Our results establish the member of this group as objects which are veryclose to the Main Sequence. This is also supported by Pre-Main Sequenceevolutionary tracks as well as by observational results. We thereforecontradict prior conclusions that most of these stars are in the middleof their Main Sequence lifetime. The new results strongly support thepredictions of the accretion theory.
| The distance to Complex M and the Intermediate Velocity Arch
The Intermediate Velocity Arch is an association of Hi clouds lyingwithin the broad limits l~110 deg-210 deg,b~50 deg-80 deg. We usehigh-resolution optical, and single-dish 21-cm, observations of 10early-type halo star sightlines in this region to establish distancelimits (0.4<=z<=3.5kpc) for seven IVCs that are part of the Arch.We re-examine a previous determination of upper and lower distancelimits on the IVC Complex M using the closely aligned halo starsBD+382182 and HD93521. Our Hi spectra show no evidence of emission fromComplex M, leading us to conclude that, while an upper distance limit ofz<=3.5 kpc may be established, no useful lower distance determinationcan be made. Our new Hi observations allow new limits to be establishedon the metallicity of Complex M, and show C, O and Si variations withrespect to solar abundances in the range +/-0.3 dex.
| A consolidated catalogue of lambda Bootis stars
lambda Bootis stars challenge our understanding of diffusion andaccretion processes related to stars and their circumstellarenvironment, and they are interesting components of the classicalinstability strip. Attempts to derive group properties with statisticalmethods are severely limited by the small number of unambiguouslyidentified lambda Bootis stars. In general, the subject appears to beobscured by incorrect memberships and it is therefore essential toprovide a sufficiently large catalogue of definitive group membersbefore modeling the lambda Bootis phenomenon. This paper describes thefirst steps towards this goal, based on our current knowledge of wellinvestigated members, leading to a concise definition of lambda Bootisstars: {Pop I hydrogen burning metal poor (except of C,N,O and S) A-typestars.} The definition does not depend on phenomenological features,like flux depressions, colour excesses, v sin i values, etc. Based on anew homogeneous catalogue with 45 lambda Bootis stars, we discussclassification criteria which can be used for a spectroscopic andphotometric all-sky survey for lambda Bootis stars in the field and inclusters of different ages. Based on observations obtained atESO-La,Silla, CTIO, Observatoire de Haute-Provence, OsservatorioAstronomico di Padua-Asiago, Univ. Toronto Southern Observatory,Observatorio do Pico dos Dias-LNA/CNPq/MCT (Brazil). Table 1 is alsoavailable 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.
| Intermediate-Velocity Gas in the North Galactic Hemisphere: H i Studies
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...457..703K&db_key=AST
| The behavior of the λ Bootis stars in the infrared.
We observed a sample of 20 λ Bootis (LB) stars in threewavelength regions in the near infrared between 7600 and 10800A. We findthat the Paschen lines correspond systematically to a spectral typewhich is later than the one attributed in the blue. By comparison with aconvenient set of MK standard stars we find that the O, Ca, C, S and Silines are weak in LB stars in varying degrees. An analysis of the 16 LBstars which we confirmed in the infrared shows that seven exhibitevidences of classical A-type shells in the spectroscopic sense. Ofthese seven, five are certain and two are dubious, giving thus apercentage of at least 30% of shells in LB stars.
| Hydrogen-line profiles of six lambda Bootis stars
Based on high resolution spectroscopic observations hydrogen-lineprofiles of six lambda Bootis stars: HD 31295, HD 101108, HD 105058, HD106223, HD 142703 and HD 183324 are presented. Peculiar line profileswith weak cores and broad but shallow wings are found for four of thestars. Influence of metallicity parameter (Z/H) and effectivetemperature on the appearance of the observed hydrogen lines isdiscussed.
| Catalogue of Lambda Bootis Candidates
Not Available
| The UV spectrum as a signature of the Lambda Bootis character
The spectra of all the stars previously classified as Lambda Bootisstars and observed by the IUE satellite at low resolution, in the shortwavelength range, are analyzed. The usefulness of this spectral rangefor classifying the Lambda Boo stars is shown; the UV criteria used todistinguish the Lambda Boo stars from other metal-deficient stars areselected and applied. The origin of the Lambda Boo phenomenon is not yetclear (Baschek and Slettebak, 1988) and a careful selection of thecandidates is the first step for a clear definition of the theoreticalproblem. From the present study, it turns out that only seven out of the19 candidates can be assigned to the Lambda Boo group, while for theother stars the previous classification must be considered eroneous. Thepeculiarities of the other metal-deficient, but not Lambda Boo, starsare discussed.
| Delta-a photometry of lambda Bootis stars
Delta-a photometry, which had been originally designed fordiscriminating magnetic peculiar stars in a vs. color diagrams, is shownto separate there lambda Bootis stars in the opposite sense, i.e. bynegative Delta-a-values indicating low metallicity as the m1-index ofStroemgren photometry, which however suffers from contamination throughH-delta effects. Controversial lambda Bootis type assignments arediscussed in connection with their Delta-a-values.
| The chemical composition of the Lambda Bootis stars
Measurements of the equivalent widhts of 24 UV lines from IUE spectra of10 ? Bootis or suspected ? Bootis stars and 19 normalstandard stars of spectral types B8-A7 are compared with line strengthscalculated from model atmospheres. The light elements (C, N, and O) inthe ? Boo stars are in the range slightly overabundant relativeto the standard (solar composition) stars. On the other hand, theheavier elements (Mg, Al, Si, S, Mn, Fe, and Ni) are moderatelydeficient (?0.5 dex) in the ? Boo stars compared to thestandard stars. The results are difficult to understand in terms ofnucleosynthesis, nor is an explanation based on a possible low-abundancefluctuation in the interstellar medium at the time of star formationvery satisfactory. A model based on the diffusion hypothesis hasattractive features, but the rapid rotation of the ? Boo starsmay present difficulties.
| Merged log of IUE observations.
Not Available
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Observation and Astrometry data
| Constellation: | Ursa Major |
| Right ascension: | 12h05m43.35s |
| Declination: | +49°40'56.0" |
| Apparent magnitude: | 8.882 |
| Distance: | 187.97 parsecs |
| Proper motion RA: | -10.1 |
| Proper motion Dec: | 1.5 |
| B-T magnitude: | 9.095 |
| V-T magnitude: | 8.9 |
Catalogs and designations:
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