Observed Orbital Eccentricities
For 391 spectroscopic and visual binaries with known orbital elementsand having B0-F0 IV or V primaries, we collected the derivedeccentricities. As has been found by others, those binaries with periodsof a few days have been circularized. However, those with periods up toabout 1000 or more days show reduced eccentricities that asymptoticallyapproach a mean value of 0.5 for the longest periods. For those binarieswith periods greater than 1000 days their distribution of eccentricitiesis flat from 0 to nearly 1, indicating that in the formation of binariesthere is no preferential eccentricity. The binaries with intermediateperiods (10-100 days) lack highly eccentric orbits.
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Tidal Effects in Binaries of Various Periods
We found in the published literature the rotational velocities for 162B0-B9.5, 152 A0-A5, and 86 A6-F0 stars, all of luminosity classes V orIV, that are in spectroscopic or visual binaries with known orbitalelements. The data show that stars in binaries with periods of less thanabout 4 days have synchronized rotational and orbital motions. Stars inbinaries with periods of more than about 500 days have the samerotational velocities as single stars. However, the primaries inbinaries with periods of between 4 and 500 days have substantiallysmaller rotational velocities than single stars, implying that they havelost one-third to two-thirds of their angular momentum, presumablybecause of tidal interactions. The angular momentum losses increase withdecreasing binary separations or periods and increase with increasingage or decreasing mass.
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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
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Does Rotation Alone Determine Whether an A-Type Star's Spectrum Is Abnormal or Normal?
As noted by Abt & Morrell, virtually all of the metallic line (Am)and peculiar A (Ap) stars have equatorial rotational velocities lessthan 120 km s-1, and most of the normal A0-F0 main-sequencestars have equatorial rotational velocities greater than 120 kms-1. However, at all spectral types there are some (10%-20%)of the normal stars that have smaller rotational velocities. If thisoverlap is real, then a star's rotational velocity is insufficient toexplain its abnormal or normal spectra. We studied the A5-F0 and A2-A4stars and found in both cases that there are stars classified as``normal'' that have unusually weak Ca II K lines and/or that occur inshort-period binaries. Therefore, the overlap seems to be due toundetected marginal abnormal stars. Among the A0-A1 stars we find thatour inability to distinguish consistently the class IV from the class Vstars can explain the overlap because the class IV stars have lowerrotational velocities than class V stars. We conclude from statisticalarguments that rotation alone can explain the appearance of an A star aseither abnormal or normal.
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The rapidly evolving hypergiant IRC +10 420: High-resolution bispectrum speckle-interferometry and dust-shell modelling
The hypergiant IRC +10 420 is a unique object for thestudy of stellar evolution since it is the only object that is believedto be witnessed in its rapid transition from the red supergiant stage tothe Wolf-Rayet phase. Its effective temperature has increased by1000-2000 K within only 20 yr. We present the first speckle observationsof IRC +10 420 with 73 mas resolution. Adiffraction-limited 2.11 mu m image was reconstructed from 6 m telescopespeckle data using the bispectrum speckle-interferometry method. Thevisibility function shows that the dust shell contributes ~ 40% to thetotal flux and the unresolved central object ~ 60%. Radiative transfercalculations have been performed to model both the spectral energydistribution and visibility function. The grain sizes, a, were found tobe in accordance with a standard distribution function, n(a) ~ a(-3.5) ,with a ranging between a_min = 0.005 mu m and a_max = 0.45 mu m. Theobserved dust shell properties cannot be fitted by single-shell modelsbut seem to require multiple components. At a certain distance weconsidered an enhancement over the assumed 1/r{(x}) densitydistribution. The best model for both SED and visibility was found for adust shell with a dust temperature of 1000 K at its inner radius of 69R_{*}. At a distance of 308 R_{*} the density was enhanced by a factorof 40 and and its density exponent was changed from x=2 to x=1.7. Theshell's intensity distribution was found to be ring-like. The ringdiameter is equal to the inner diameter of the hot shell ( ~ 69 mas).The diameter of the central star is ~ 1 mas. The assumption of a hotterinner shell of 1200 K gives fits of almost comparable quality butdecreases the spatial extension of both shells' inner boundaries by ~30% (with x=1.5 in the outer shell). The two-component model can beinterpreted in terms of a termination of an enhanced mass-loss phaseroughly 60 to 90 yr (for d=5 kpc) ago. The bolometric flux, F_bol, is8.17 * 10(-10) Wm(-2) corresponding to a central-star luminosity ofL/Lsun = 25 462 * (d/kpc)(2) .
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Mass determination of astrometric binaries with Hipparcos. II. Selection of candidates and results
In a previous paper (\cite{Mar97}) we have shown that for double starswith orbital periods smaller than about 25 years, it was possible todetermine from the Hipparcos data, the mass ratio B of the components orthe difference between the mass and intensity ratios, beta -B, providedthe orbital elements of the relative orbit are available. From anextensive literature search we have selected 145 potential systems, ofwhich 46 yielded eventually a satisfactory solution. For eight systemswith the largest separations, the peculiarities of the natural directionassociated to the Hipparcos observations, the 'hippacentre', have beenfully exploited to derive the mass ratio of the components without anyadditional assumption. For the remaining 38, the derivation of the massratio was possible only by taking the magnitude difference between thetwo components from other sources. The parallax determinedsimultaneously, is then used to produce the individual masses of thecomponents. The astrophysical relevance of the results is discussed andwhen possible (17 systems) the masses are compared to ground-basedvalues.
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Mass determination of astrometric binaries with Hipparcos. I. Theory and simulation
The analysis of the observations of double stars made by the ESAsatellite Hipparcos has involved a very specific processing to derivethe relevant astrometric parameters. This required to distinguishbetween several categories of double stars according to the separationand orbital motion. We show that for close pairs with orbital periodless than about 20 years, the concept of photocentric orbit of anastrometric binary needs to be generalized to benefit fully from theaccuracy of Hipparcos. We introduce a point more naturally associatedwith the Hipparcos observations, the hippacentre, whose orbital path isnot longer similar to the relative keplerian orbit of the components,unlike that of the photocentre. For systems with separation larger thanabout 0.3", it is possible to determine separately the mass and theintensity ratio of the components from the absolute path of thehippacentre on the sky. For smaller separations the scale of thephotocentric orbit is recovered as a limiting case. The scope of thispaper is to set forth the principles of the method and to explore itspossibilities and limitations from extensive simulations. Based onobservations made by the ESA Hipparcos satellite.
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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
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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.
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ICCD speckle observations of binary stars. VIII - Measurements during 1989-1991 from the Cerro Tololo 4 M telescope
One-thousand eighty-eight observations of 947 binary star systems,observed by means of speckle interferometry with the 4 m telescope onCerro Tololo, are presented. These measurements, made during the period1989-1991, comprise the second installment of results stemming from theexpansion of our speckle program to the southern hemisphere.
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Optical Polarization of 1000 Stars Within 50-PARSECS from the Sun
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&AS..101..551L&db_key=AST
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A Polarimetric Investigation on Interstellar Dust Within 50-PARSECS from the Sun
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&A...274..203L&db_key=AST
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ICCD speckle observations of binary stars. IV - Measurements during 1986-1988 from the Kitt Peak 4 M telescope
One thousand five hundred and fifty measurements of 1006 binary starsystems observed mostly during 1986 through mid-1988 by means of speckleinterferometry with the KPNO 4-m telescope are presented. Twenty-onesystems are directly resolved for the first time, including newcomponents to the cool supergiant Alpha Her A and the Pleiades shellstar Pleione. A continuing survey of The Bright Star Catalogue yieldedeight new binaries from 293 bright stars observed. Corrections tospeckle measures from the GSU/CHARA ICCD speckle camera previouslypublished are presented and discussed.
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Starbursts, binary stars, and blue stragglers in local superclusters and groups. I - The very young disk and young disk populations
The distributions in the HR diagram with theoretical time-constant locifor stars in several young clusters and superclusters are compared todemonstrate that 'blue stragglers' in these aggregates are mostfrequently simply single massive (mode B) stars formed in bursts of starformation that occur at discrete intervals in time following theformation of the bulk of the low-mass (mode A) stars in the aggregate.The characteristics of the close binary systems in these aggregates areexamined to show that, in several cases, mass transfer by Roche lobeoverflow has or will occur and that, in some instances, the system wouldhave appeared as a blue straggler prior to the mass-transfer event, and,in other instances, mass transfer will lead to the identification of thesystem as a blue straggler. Thus, it is concluded that the bluestraggler phenomenon has at least two distinct physical origins: it mayoriginate from delayed formation (starbursts) or from 'delayedevolution' in some close binaries (mass transfer from an evolvedprimary).
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Interferometric Observations of Double Stars in 1985 and 1986
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1988A&AS...72..563T&db_key=AST
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ICCD speckle observations of binary stars. I - A survey for duplicity among the bright stars
A survey of a sample of 672 stars from the Yale Bright Star Catalog(Hoffleit, 1982) has been carried out using speckle interferometry onthe 3.6-cm Canada-France-Hawaii Telescope in order to establish thebinary star frequency within the sample. This effort was motivated bythe need for a more observationally determined basis for predicting thefrequency of failure of the Hubble Space Telescope (HST) fine-guidancesensors to achieve guide-star lock due to duplicity. This survey of 426dwarfs and 246 evolved stars yielded measurements of 52 newly discoveredbinaries and 60 previously known binary systems. It is shown that thefrequency of close visual binaries in the separation range 0.04-0.25arcsec is 11 percent, or nearly 3.5 times that previously known.
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A systematic search for members of the Hyades Supercluster. IV - The metallic-line stars and ultrashort-period Cepheids
Bright Star Catalog stars with beta values in the 2.70-2.88 rangecontain 127 members of the Hyades Supercluster, which have been chosenon the basis of the direction of their proper motion. Available radialvelocities confirm supercluster membership for most of these stars.Exceptional regularity is noted in the values of the pulsation constantQ computed for the ultrashort period Cepheids on the basis of knownperiods, model masses and model radii. Outside the center of the Hyadescluster, the largest concentration of supercluster stars is in a regionof 30 pc radius, between 60 and 80 pc above the sun, where 30 percent ofthe expected stars in the temperature range presently discussed aresupercluster members.
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Speckle interferometric measurements of binary stars. IX
Four hundred-forty measurements of 232 binary stars observed during 1981by means of speckle interferometry with the 4-m telescope at KPNO arerepresented. Newly resolved systems include Xi-1 Cet, Rho Her A, HD187321, and 59 Cyg A.
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A Systematic Search for Members of the Hyades Supercluster - Part Two - the Visual Binaries
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1984AJ.....89..839E&db_key=AST
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Speckle interferometric measurements of binary stars. VIII
Six hundred measurements of 331 binary stars observed during 1980 bymeans of speckle interferometry with the 4 m telescope at Kitt PeakNational Observatory are presented. Thirty-two systems are directlyresolved for the first time. Newly resolved spectroscopic binariesinclude HR 2001, 53 Dam, HR 6388, HR 6469, 31 Omicron-2 Cyg, HR 7922,and alpha Equ.
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Supplement to the Second Catalogue of Am Stars with Known Spectral Types (end 1981)
Not Available
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The Hyades main sequence
Intermediate band, H-beta and RI observations of 72 Hyades cluster starsto V = 11 mag are reported and discussed. A modulus of 3.2 mag isderived on the basis of a comparison with field stars of large parallax.Also presented are observations of 98 main-sequence stars of the Hyadesgroup that were previously found to be group members from kinematicalconsiderations. Parallaxes of the group stars, computed on theassumption that they are members of an extended Hyades cluster, yieldmean values of (U, V, W) = (+40.5, -18.4, -4.9) km/s, with dispersionsof (2.3, 2.3, 6.0) km/s, compared with (+41.7, -18.4, -2.0) and (2.6,1.3, 1.9) km/s for the brightest cluster members. It is noted that allthe stars discussed can be considered as members of a supercluster inwhich only a slight relaxation control of the W velocities is presentfor stars far from the nucleus. Evidence is found, including that of thePraesepe cluster at Z = +80 pc, for some interchange between the U, V,and W velocities in stars farthest from the galactic plane, with thetotal cluster velocity being maintained.
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Visual multiples. VII - MK classifications
Classifications are given for 865 components of visual multiples; theyshow no systematic differences from the MK system, and the random errorsare one subclass in type and two-thirds of a luminosity class. It isfound that at least 1% of the F-type IV and V stars are weak-lined, 32%of the A4-F1 IV and V stars are Am, and 5% of the A0-A3 IV and V starsare early-type Am. Attention is called to the large fraction (55%) ofthe A3-A9 III-V stars that are of luminosity classes III or IV, unlikethe percentage (16%) at neighboring types.
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Visual multiples. V - Radial velocities of 160 systems
937 radial velocities are listed from coude spectra of 160 visualmultiples with known visual orbital elements; these, plus the velocitiesin paper of Roemer and Sanwal (1980), are discussed. Among the resultsare (1) systems yielding spectroscopic elements with the visual period,(2) systems probably showing velocity variations during the visualperiod, (3) systems with short spectroscopic periods, some in additionto detectable motion during the visual period, (4) systems showing novariation in radial velocity during the visual period, either becausethe components are similar in brightness or the periods are very long,(5) systems with spectral lines too broad to allow the detection oforbital motion, and (6) systems with insufficient data for anyconclusions to be drawn at present.
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Speckle interferometric measurements of binary stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1980A&AS...42..185B&db_key=AST
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A photometric study of some AM stars
Not Available
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A survey for southern Delta Scuti variable stars
Twenty-nine field stars have been tested photoelectrically forshort-period variability. Eighteen of these stars have spectral typesbetween A2 and F5 and are not Am stars; of these, six have beendiscovered to be variable and one is a suspected variable. HD 185969,with a period of 0.361 day, has the longest known period for a star ofthe Delta Scuti type. The predominance of discovered variables withamplitudes close to the detection limit is suggestive of most stars inthe instability strip being pulsators.
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Photometry of AM stars
Not Available
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Absolute luminosity calibration of Stroemgren's 'late group'
A statistical parallax method based on the principle of maximumlikelihood is used to calibrate absolute luminosities for samples ofcooler stars constituting the 'late group' defined by Stromgren (1966).The samples examined include 415 stars of all luminosity classes and asubset comprising 86 main-sequence stars. Linear calibration relationsinvolving the Stromgren beta, (b-y), and bracketted c1 indices arederived which yield mean absolute magnitudes with an accuracy of 0.09magnitude for the overall sample and 0.13 magnitude for themain-sequence subsample. Several second-order relations are considered,and the results are compared with Crawford's (1975) calibrations as wellas with mean absolute magnitudes obtained from trigonometric parallaxes.The possible effect of interstellar absorption on the calibrationrelations is also investigated.
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On the inclination of rotation axes in visual binaries.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974ApJ...190..331W&db_key=AST
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