Contenidos
Imágenes
Subir su imagen
DSS Images Other Images
Artículos relacionados
A 40 Myr Old Gaseous Circumstellar Disk at 49 Ceti: Massive CO-rich Comet Clouds at Young A-type Stars
The gaseous molecular disk that orbits the main-sequence A-type star 49Ceti has been known since 1995, but the stellar age and the origin ofthe observed carbon monoxide molecules have been unknown. We nowidentify 49 Ceti as a member of the 40 Myr old Argus Association andpresent a colliding comet model to explain the high CO concentrationsseen at 49 Ceti and the 30 Myr old A-type star HD 21997. The modelsuggests that massive—400 Earth mass—analogs of the Sun'sKuiper Belt are in orbit around some A-type stars, that these largemasses are composed primarily of comet-like objects, and that theseobjects are rich in CO and perhaps also CO2. We identifyadditional early-type members of the Argus Association and theTucana/Horologium and Columba Associations; some of these stars displayexcess mid-infrared emission as measured with the Widefield InfraredSurvey Explorer.
| The International Deep Planet Survey. I. The frequency of wide-orbit massive planets around A-stars
Breakthrough direct detections of planetary companions orbiting A-typestars confirm the existence of massive planets at relatively largeseparations, but dedicated surveys are required to estimate thefrequency of similar planetary systems. To measure the first estimationof the giant exoplanetary systems frequency at large orbital separationaround A-stars, we have conducted a deep-imaging survey of young (8-400Myr), nearby (19-84 pc) A- and F-stars to search for substellarcompanions in the ~10-300 AU range. The sample of 42 stars combines allA-stars observed in previous AO planet search surveys reported in theliterature with new AO observations from VLT/NaCo and Gemini/NIRI. Itrepresents an initial subset of the International Deep Planet Survey(IDPS) sample of stars covering M- to B-stars. The data were obtainedwith diffraction-limited observations in H- and Ks-bandcombined with angular differential imaging to suppress the speckle noiseof the central stars, resulting in typical 5? detection limits inmagnitude difference of 12 mag at 1'', 14 mag at 2'' and 16 mag at 5''which is sufficient to detect massive planets. A detailed statisticalanalysis of the survey results is performed using Monte Carlosimulations. Considering the planet detections, we estimate the fractionof A-stars having at least one massive planet (3-14 MJup) inthe range 5-320 AU to be inside 5.9-18.8% at 68% confidence, assuming aflat distribution for the mass of the planets. By comparison, the browndwarf (15-75 MJup) frequency for the sample is 2.0-8.9% at68% confidence in the range 5-320 AU. Assuming power law distributionsfor the mass and semimajor axis of the planet population, the AO dataare consistent with a declining number of massive planets withincreasing orbital radius which is distinct from the rising slopeinferred from radial velocity (RV) surveys around evolved A-stars andsuggests that the peak of the massive planet population around A-starsmay occur atseparations between the ranges probed by existing RV and AOobservations. Finally, we report the discovery of three new close M-starcompanions to HIP 104365 and HIP 42334.Based on observations collected at the European Southern Observatory,Chile, ESO programs 081.C-0519, 083.C-0706, 084.C-0605, 087.C-0559,088.C-0477, and at the Gemini North observatory, Gemini programsGN-2007B-Q-59, GN-2008A-Q-77, GN-2008B-Q-64, GN-2009A-Q-80,GN-2009B-Q-93.Table A.1 is available in electronic form at http://www.aanda.orgTables 1, 3, and A.1are also available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/544/A9
| Rotational velocities of A-type stars. IV. Evolution of rotational velocities
Context. In previous works of this series, we have shown that late B-and early A-type stars have genuine bimodal distributions of rotationalvelocities and that late A-type stars lack slow rotators. Thedistributions of the surface angular velocity ratio?/?crit (?crit is the criticalangular velocity) have peculiar shapes according to spectral typegroups, which can be caused by evolutionary properties. Aims: Weaim to review the properties of these rotational velocity distributionsin some detail as a function of stellar mass and age. Methods: Wehave gathered vsini for a sample of 2014 B6- to F2-type stars. We havedetermined the masses and ages for these objects with stellar evolutionmodels. The (Teff,log L/L&sun;)-parameters weredetermined from the uvby-? photometry and the HIPPARCOS parallaxes. Results: The velocity distributions show two regimes that dependon the stellar mass. Stars less massive than 2.5 M&sun; havea unimodal equatorial velocity distribution and show a monotonicalacceleration with age on the main sequence (MS). Stars more massive havea bimodal equatorial velocity distribution. Contrarily to theoreticalpredictions, the equatorial velocities of stars from about 1.7M&sun; to 3.2 M&sun; undergo a strong accelerationin the first third of the MS evolutionary phase, while in the last thirdof the MS they evolve roughly as if there were no angular momentumredistribution in the external stellar layers. The studied stars mightstart in the ZAMS not necessarily as rigid rotators, but with a totalangular momentum lower than the critical one of rigid rotators. Thestars seem to evolve as differential rotators all the way of their MSlife span and the variation of the observed rotational velocitiesproceeds with characteristic time scales ?t ? 0.2tMS, where tMS is the time spent by a star in theMS.Full Table 1 is only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/537/A120Appendicesare available in electronic form at http://www.aanda.org
| The star catalogue of Hevelius. Machine-readable version and comparison with the modern Hipparcos Catalogue
The catalogue by Johannes Hevelius with the positions and magnitudes of1564 entries was published by his wife Elisabeth Koopman in 1690. Weprovide a machine-readable version of the catalogue, and briefly discussits accuracy on the basis of comparison with data from the modernHipparcos Catalogue. We compare our results with an earlier analysis byRybka (1984), finding good overall agreement. The magnitudes given byHevelius correlate well with modern values. The accuracy of his positionmeasurements is similar to that of Brahe, with ? = 2´ forlongitudes and latitudes, but with more errors >5´ thanexpected for a Gaussian distribution. The position accuracy decreasesslowly with magnitude. The fraction of stars with position errors largerthan a degree is 1.5%, rather smaller than the fraction of 5% in thestar catalogue of Brahe.Star catalogue of Hevelius is only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A29
| Three editions of the star catalogue of Tycho Brahe. Machine-readable versions and comparison with the modern Hipparcos Catalogue
Tycho Brahe completed his catalogue with the positions and magnitudes of1004 fixed stars in 1598. This catalogue circulated in manuscript form.Brahe edited a shorter version with 777 stars, printed in 1602, andKepler edited the full catalogue of 1004 stars, printed in 1627. Weprovide machine-readable versions of the three versions of thecatalogue, describe the differences between them and briefly discusstheir accuracy on the basis of comparison with modern data from theHipparcos Catalogue. We also compare our results with earlier analysesby Dreyer (1916, Tychonis Brahe Dani Scripta Astronomica, Vol. II) andRawlins (1993, DIO, 3, 1), finding good overall agreement. Themagnitudes given by Brahe correlate well with modern values, hislongitudes and latitudes have error distributions with widths of2´, with excess numbers of stars with larger errors (as comparedto Gaussian distributions), in particular for the faintest stars. Errorsin positions larger than ?10´, which comprise about 15% ofthe entries, are likely due to computing or copying errors.The full tables KeplerE and Variants (see Table 4) and the table withthe latin descriptions of the stars are available in electronic formonly at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A28
| The PASTEL catalogue of stellar parameters
Aims: The PASTEL catalogue is an update of the [Fe/H] catalogue,published in 1997 and 2001. It is a bibliographical compilation ofstellar atmospheric parameters providing (T_eff, log g, [Fe/H])determinations obtained from the analysis of high resolution, highsignal-to-noise spectra, carried out with model atmospheres. PASTEL alsoprovides determinations of the one parameter T_eff based on variousmethods. It is aimed in the future to provide also homogenizedatmospheric parameters and elemental abundances, radial and rotationalvelocities. A web interface has been created to query the catalogue onelaborated criteria. PASTEL is also distributed through the CDS databaseand VizieR. Methods: To make it as complete as possible, the mainjournals have been surveyed, as well as the CDS database, to findrelevant publications. The catalogue is regularly updated with newdeterminations found in the literature. Results: As of Febuary2010, PASTEL includes 30151 determinations of either T_eff or (T_eff,log g, [Fe/H]) for 16 649 different stars corresponding to 865bibliographical references. Nearly 6000 stars have a determination ofthe three parameters (T_eff, log g, [Fe/H]) with a high qualityspectroscopic metallicity.The catalogue can be queried through a dedicated web interface at http://pastel.obs.u-bordeaux1.fr/.It is also available in electronic form at the Centre de DonnéesStellaires in Strasbourg (http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/pastel),at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) orvia http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/515/A111
| Catalogue of Ap, HgMn and Am stars
We present a catalogue of 8205 known or suspected Ap, HgMn and Am stars.This paper is a major update of our first edition of the catalog of Apand Am stars and includes revised identifications, additional stars andrevised information obtained from the literature.Catalogue (full Table 1) is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/498/961
| A catalogue of multiplicity among bright stellar systems
We consider the multiplicity of stellar systems with (combined)magnitude brighter than 6.00 in Hipparcos magnitudes. We identify 4559such bright systems (including the Sun), and the frequencies ofmultiplicities 1, 2,..., 7 are found to be 2718, 1437, 285, 86, 20, 11and 2. We discuss the uncertainties, which are substantial. We alsoconsider the distributions of periods of orbits and suborbits. We notethat for even more restricted set of 478 systems with VH<= 4.00, the proportions of higher multiples up to sextuple areprogressively larger (213, 179, 54, 19, 8, 5), suggesting substantialincompleteness in even the reasonably well studied larger sample.This sample can be seen as relatively thoroughly studied formultiplicity, and reasonably representative of stars more massive thanthe Sun. But the restriction to VH <= 6 means that oursample contains hardly any systems where all components are low-massmain-sequence stars (K or M).Data on multiplicity are important as a constraint on (i) the starformation problem, (ii) the problem of the evolution of the Galacticstellar population and (iii) the interaction of dynamics and evolutionthrough the effect of Kozai cycles. We discuss these topics briefly.
| Rotational velocities of A-type stars. III. Velocity distributions
Aims.A sample of v sin i of B9 to F2-type main sequence single stars hasbeen built from highly homogeneous {v sin i} parameters determined for alarge sample cleansed of objects presenting the Am and Ap phenomenon aswell as of all known binaries. The aim is to study the distributions ofrotational velocities in the mass range of A-type stars for normalsingle objects. Methods: .Robust statistical methods are used torectify the {v sin i} distributions for the projection effect and theerror distribution. The equatorial velocity distributions are obtainedfor about 1100 stars divided in six groups defined by the spectral type,under the assumption of randomly orientated rotational axes.Results: .We show that late B and early A-type main-sequence stars havegenuine bimodal distributions of true equatorial rotational velocitiesprobably due to angular momentum loss and redistribution that the starunderwent before reaching the main sequence. A striking lack of slowrotators is noticed among intermediate and late A-type stars.Full Table [see full text] is only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/463/671 Appendices areonly available in electronic form at http://www.aanda.org
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| 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.
| Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i
This work is the second part of the set of measurements of v sin i forA-type stars, begun by Royer et al. (\cite{Ror_02a}). Spectra of 249 B8to F2-type stars brighter than V=7 have been collected at Observatoirede Haute-Provence (OHP). Fourier transforms of several line profiles inthe range 4200-4600 Å are used to derive v sin i from thefrequency of the first zero. Statistical analysis of the sampleindicates that measurement error mainly depends on v sin i and thisrelative error of the rotational velocity is found to be about 5% onaverage. The systematic shift with respect to standard values fromSlettebak et al. (\cite{Slk_75}), previously found in the first paper,is here confirmed. Comparisons with data from the literature agree withour findings: v sin i values from Slettebak et al. are underestimatedand the relation between both scales follows a linear law ensuremath vsin inew = 1.03 v sin iold+7.7. Finally, thesedata are combined with those from the previous paper (Royer et al.\cite{Ror_02a}), together with the catalogue of Abt & Morrell(\cite{AbtMol95}). The resulting sample includes some 2150 stars withhomogenized rotational velocities. Based on observations made atObservatoire de Haute Provence (CNRS), France. Tables \ref{results} and\ref{merging} are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/897
| 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
| Sixth Catalogue of Fundamental Stars (FK6). Part III. Additional fundamental stars with direct solutions
The FK6 is a suitable combination of the results of the HIPPARCOSastrometry satellite with ground-based data, measured over a longinterval of time and summarized mainly in the FK5. Part III of the FK6(abbreviated FK6(III)) contains additional fundamental stars with directsolutions. Such direct solutions are appropriate for single stars or forobjects which can be treated like single stars. Part III of the FK6contains in total 3272 stars. Their ground-based data stem from thebright extension of the FK5 (735 stars), from the catalogue of remainingSup stars (RSup, 732 stars), and from the faint extension of the FK5(1805 stars). From the 3272 stars in Part III, we have selected 1928objects as "astrometrically excellent stars", since their instantaneousproper motions and their mean (time-averaged) ones do not differsignificantly. Hence most of the astrometrically excellent stars arewell-behaving "single-star candidates" with good astrometric data. Thesestars are most suited for high-precision astrometry. On the other hand,354 of the stars in Part III are Δμ binaries in the sense ofWielen et al. (1999). Many of them are newly discovered probablebinaries with no other hitherto known indication of binarity. The FK6gives, besides the classical "single-star mode" solutions (SI mode),other solutions which take into account the fact that hidden astrometricbinaries among "apparently single-stars" introduce sizable "cosmicerrors" into the quasi-instantaneously measured HIPPARCOS proper motionsand positions. The FK6 gives, in addition to the SI mode, the "long-termprediction (LTP) mode" and the "short-term prediction (STP) mode". TheseLTP and STP modes are on average the most precise solutions forapparently single stars, depending on the epoch difference with respectto the HIPPARCOS epoch of about 1991. The typical mean error of anFK6(III) proper motion in the single-star mode is 0.59 mas/year. This isa factor of 1.34 better than the typical HIPPARCOS errors for thesestars of 0.79 mas/year. In the long-term prediction mode, in whichcosmic errors are taken into account, the FK6(III) proper motions have atypical mean error of 0.93 mas/year, which is by a factor of about 2better than the corresponding error for the HIPPARCOS values of 1.83mas/year (cosmic errors included).
| 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.
| The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS...99..135A&db_key=AST
| The general catalogue of trigonometric [stellar] paralaxes
Not Available
| The position corrections of 1400 stars observed with PA II in San Juan.
Not Available
| Newly identified main-sequence A stars with circumstellar dust
The IRAS Faint Source Survey data base and the ADDSCAN/SCANPI softwareare used to search for systems with circumstellar dust in two samples:all of the 62 A stars in Woolley's catalog, which lie near the mainsequence and are typically within 25 pc of the sun, and all A stars inthe Bright Star Catalogue with mV in the range 4-5 and v sin i not lessthan 100 km/s. In the first sample, 11 nearby A stars having (12)-(25)and (25)-(60) colors consistent with circumstellar dust are found. Theanalysis of the second sample demonstrates that the use of the FSS database increases the likelihood of identifying A stars with circumstellardust fainter than mV = 4. Three more new dusty systems are found in thissample. Beta Pictoris (A5 IV-V) is the only star within 25 pc of the sunthat displays IR colors indicative of both warm and cool dust. It isinferred from the absence of cool dust in the vast majority of thesystems that the dust disks of these stars are much less extended thanthat seen around Beta Pictoris.
| General catalogue of AP and AM stars
A catalog of all the known Ap and Am stars, containing a total of 6684objects, was prepared. The few stars that were wrongly considered as Apor Am star are noted as well as some others for which their identity asAp or Am stars is not yet well established. The catalog gives theidentificators and the main observational data for each star, includingthe magnitude, color, spectral type, duplicity, periodicity, magneticfield, and projected rotational velocity.
| CA II H and K measurements made at Mount Wilson Observatory, 1966-1983
Summaries are presented of the photoelectric measurements of stellar CaII H and K line intensity made at Mount Wilson Observatory during theyears 1966-1983. These results are derived from 65,263 individualobservations of 1296 stars. For each star, for each observing season,the maximum, minimum, mean, and variation of the instrumental H and Kindex 'S' are given, as well as a measurement of the accuracy ofobservation. A total of 3110 seasonal summaries are reported. Factorswhich affect the ability to detect stellar activity variations andaccurately measure their amplitudes, such as the accuracy of the H and Kmeasurements and scattered light contamination, are discussed. Relationsare given which facilitate intercomparison of 'S' values with residualintensities derived from ordinary spectrophotometry, and for convertingmeasurements to absolute fluxes.
| Fifth fundamental catalogue. Part 2: The FK5 extension - new fundamental stars
The mean positions and proper motions for 3117 new fundamental starsessentially in the magnitude range about 4.5 to 9.5 are given in thisFK5 extension. Mean apparent visual magnitude is 7.2 and is on average2.5 magnitudes fainter then the basic FK5 which has a mean magnitude of4.7. (The basic FK5 gives the mean positions and proper motions for theclassical 1535 fundamental stars). The following are discussed: theobservational material, reduction of observations, star selection, andthe system for the FK5 extension. An explanation and description of thecatalog are given. The catalog of 3117 fundamental stars for the equinoxand epoch J2000.0 and B1950.0 is presented. The parallaxes and radialvelocities for 22 extension stars with large forecasting effects aregiven. Catalogs used in the compilation of the FK5 fundamental catalogare listed.
| The early A type stars - Refined MK classification, confrontation with Stroemgren photometry, and the effects of rotation
The MK classification system for the early A-type stars is refined, anda parallel system of standards for the broad-lined stars is introduced.With this improved system, stars may be classified with significantlygreater precision than before. It is shown that spectral types in thissystem are not systematically affected by rotational line broadening. Atotal of 372 early A-type stars are classified, and a confrontation ofthese spectral types with Stroemgren photometry reveals a number ofsystematic photometric effects of rotation. In particular, high v sin istars are systematically redder than low v sin i stars of the samespectral type, and the beta index is weakened by rotation. It isconcluded that precise spectral classification in conjunction withStroemgren and H-beta photometry can potentially provide a valuablecheck and input to the theory of the atmospheres of rotating stars.
| Corrections to or comments on errata contributed by E. H. Olsen in Bull. Inform. CDS 26, 69 (1984)
Not Available
| Photoelectric observations of lunar occultations. XV
The last (or possibly penultimate) paper in a series on lunaroccultations presents observations of 404 phenomena, preceded by somegeneral remarks of a retrospective nature. The series of observationsbegan in 1968. Data for 20 doubles or suspected doubles are presented,ranked in order of certainty, with designation 3 representing thesurest. Thirteen of the cases refer to stars not previously noted asdoubles. Seven determinations of angular diameters are presented, ofwhich three have been previously observed.
| The local system of early type stars - Spatial extent and kinematics
Published uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter.
| A study of delta/1400/-Ap stars
Delta-a photometry was carried out for 10 stars for which excess valuesof the UV index delta(1400) had been found. The study confirmedpronounced peculiarity for the two hottest stars and yielded mildpeculiarity for three other objects; the other members of the samplewere normal A-type stars. Results indicate a strong increase of thethreshold level of peculiarity from delta(1400) equals 0.2 mag at b-yequals -0.05 mag to delta(1400) equals 0.5 mag at b-y equals 0.0 mag. Avery good correlation between delta(1400) and Delta-a for hot Ap starsis found.
| Space velocities and ages of nearby early-type stars
Photometric distances and space velocities have been calculated for 458B0-A0 stars with apparent magnitudes not exceeding 6.5. UsingStromgren's ubvy-beta photometry the effective temperature and theposition in bolometric magnitude over the zero-age main sequence of thestars were derived. These quantities were used to obtain age and massfor 423 of the stars by interpolation in the models of stellar evolutionfor the chemical composition (X Z) = (0.7, 0.03). A relation forderiving interstellar reddening for normal stars in the intermediategroup is given.
| Absolute ultraviolet spectrophotometry from the TD1 satellite. X - The ultraviolet spectrum of the AP stars
The UV Bright Star Spectrophotometric Catalog, developed withobservations from the TD-1 satellite, provides data for comparing 77 Apstars with 344 normal stars in the ultraviolet from 1350 to 2550 A. TheBalmer and Paschen continua in the Ap stars are connected by means of along basis (2100 versus 5500 A) index. For discriminating Ap stars fromnormal ones, as well as for detecting new Ap stars, a flux deficiency at1400 A proves to be very valuable; the 1400 A feature appears to stemeither from Fe II lines in cooler Ap stars or from Si II autoionization.Domination of the Si and SrCrEu star spectra by metallic lines is alsodiscussed.
|
Enviar un nuevo artículo
Enlaces relacionados
- - No se han encontrado enlaces -
En viar un nuevo enlace
Miembro de los siguientes grupos:
|
Datos observacionales y astrométricos
| Constelación: | Capricornio |
| Ascensión Recta: | 21h08m33.61s |
| Declinación: | -21°11'36.7" |
| Magnitud Aparente: | 5.315 |
| Movimiento Propio en Ascensión Recta: | 0 |
| Movimiento Propio en Declinación: | 0 |
| B-T magnitude: | 5.326 |
| V-T magnitude: | 5.316 |
Catálogos y designaciones:
|
