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Composite spectra Paper 15: HD 216572, a triple system containing a short-period, double-lined secondary
We analyse 81 optical spectra of the composite-spectrum binary HD216572, and show that the primary is a cool giant of type G8III whilethe secondary is a double-lined binary consisting of two nearlyidentical B9 dwarfs in a 1.18-d orbit. The inner system undergoespartial eclipses, whose photometry we model to derive the physicalparameters of both secondary stars. The outer system does not eclipse.We isolate the combined spectrum of the secondary by spectralsubtraction, and from 48 separate radial-velocity measurements of bothsecondary components we obtain a triple-lined orbit solution from whichwe determine the individual masses of all three stars and theinclinations of both the inner and the outer orbits. The period of theouter system is 55 d, which is surprisingly short for a giant star, andour detection of small but non-negligible amounts of variablechromospheric emission in the CaII K line is not unlike that detected inother systems with comparably short periods. The secondary componentsare in a circular orbit and are rotating at about 95 +/- 10 kms-1 although their surface-to-surface separation is only 4Rsolar the stars are not noticeably distorted geometricallyby such close proximity. All three stars appear to be in synchronousrotation in their respective orbits. We derive fairly accurateHertzsprung-Russell diagram positions for all three stars and comparethem to evolutionary tracks calculated for the respective stellarmasses, but cannot reconcile the age of the cool giant with that of theB stars.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| A catalogue of eclipsing variables
A new catalogue of 6330 eclipsing variable stars is presented. Thecatalogue was developed from the General Catalogue of Variable Stars(GCVS) and its textual remarks by including recently publishedinformation about classification of 843 systems and making correspondingcorrections of GCVS data. The catalogue1 represents thelargest list of eclipsing binaries classified from observations.
| Composite spectra Paper 13: 93 Leonis, a chromospherically-active binary
We isolate the spectrum of the secondary component of thecomposite-binary system 93 Leonis by spectrum subtraction, classify it,and measure the mass ratio of the system. An accurate visual orbit and awell-determined parallax provide reliable measurements of orbitalinclination and distance, enabling us to determine precisely theindividual masses and other stellar parameters. The primary star is oftype ~G7 III, and the secondary is a rapidly rotating star of type A7IV. Our photographic spectra at 10 Å mm-1 areinvaluable for accurate spectral classification in such cases.By combining 23 measurements of the secondary's velocity with 102 of theprimary's and deriving a double-lined orbit, we determine the mass ratio(q=M1/M2) of 93 Leo to be 1.09 +/- 0.04. The samevalue is derived by cross-correlating high-dispersion spectra of 93 LeoB extracted from opposite nodal phases. That value of q is consonantwith previous research, but its precision is considerably improved. Weshow that random errors arising from the cross-correlation of broad,weak features constitute a natural limit to that precision.The derived masses of M1= 2.2 Msolar,M2= 2.0 Msolar for the giant and dwarf,respectively, constrain the choice of models for fitting evolutionarytracks in the (logTeff, logL) plane. The giant is almostcertainly on its first ascent of the red giant branch, and the dwarf hasevolved significantly from the main sequence. The stars fit an isochronefor log(age) = 8.95, about 0.9 Gyr. Metallicity near to solar issuggested by the close correspondence between the component spectra andthose of the respective solar-abundance standards.The primary in 93 Leo displays a marked level of chromospheric activity.By combining our high-dispersion spectra we are able to isolate emissionin the Ca II K line. The chromospheric material has a small infallvelocity, giving rise to a disc-averaged redshift of about 4 kms-1, and an unchanging velocity profile which can beattributed to a large number of small, active events like prominencesacross the surface. While we can say that there was no perceptiblechange in the emission strength over an interval of 4 months, we havenot made systematic observations to monitor its long-term stability.We contrast the components of 93 Leo with those of α Equ, whoseanalysis was the subject of Paper 11 in this series. The primarycomponents are very similar, but the two secondary components areextremely different in nature: whereas 93 Leo B is a broad-lined,apparently normal A star, the secondary of α Equ is a sharp-linedAm star of type ~kA3hA4mA9. We question why that should be, andrecommend that a greater emphasis be placed on extracting accuratestellar parameters from the components of spectroscopic binaries as ameans towards a better understanding of the vagaries of stellarevolution.93 Leo has a 9-mag visual companion which appears to be a physicalmember of the system and to be a single-lined spectroscopic binary witha period of the order of a century.
| The Vienna-KPNO search for Doppler-imaging candidate stars. I. A catalog of stellar-activity indicators for 1058 late-type Hipparcos stars
We present the results from a spectroscopic Ca ii H&K survey of 1058late-type stars selected from a color-limited subsample of the Hipparcoscatalog. Out of these 1058 stars, 371 stars were found to showsignificant H&K emission, most of them previously unknown; 23% withstrong emission, 36% with moderate emission, and 41% with weak emission.These spectra are used to determine absolute H&K emission-linefluxes, radial velocities, and equivalent widths of theluminosity-sensitive Sr ii line at 4077 Ä. Red-wavelengthspectroscopic and Strömgren y photometric follow-up observations ofthe 371 stars with H&K emission are used to additionally determinethe absolute Hα -core flux, the lithium abundance from the Li i6708 Å equivalent width, the rotational velocity vsin i, theradial velocity, and the light variations and its periodicity. Thelatter is interpreted as the stellar rotation period due to aninhomogeneous surface brightness distribution. 156 stars were found withphotometric periods between 0.29 and 64 days, 11 additional systemsshowed quasi-periodic variations possibly in excess of ~50 days. Further54 stars had variations but no unique period was found, and four starswere essentially constant. Altogether, 170 new variable stars werediscovered. Additionally, we found 17 new SB1 (plus 16 new candidates)and 19 new SB2 systems, as well as one definite and two possible new SB3systems. Finally, we present a list of 21 stars that we think are mostsuitable candidates for a detailed study with the Doppler-imagingtechnique. Tables A1--A3 are 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/Abstract.html
| 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
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| A preliminary compilation of DS-programme star positions
A catalog is presented of the double-star-program (DS-program) starpositions, listing right ascensions for 930 DSs and declinations for1225 DSs of the program. The positions were compiled from the observedvalues obtained between 1980 and 1987 with the meridian circles of sixUSSR observatories (the Moscow, Kazan', Kiev, Khar'kov, Odessa, andTashkent Observatories) and the Belgrade Observatory. The measurementsand the treatment of the observational material were performed using therelative method, and the FK-4 system stars were used as reference stars.
| Composite spectra. V - Orbital elements for 30 systems
A comprehensive survey of bright composite-spectrum binaries in thenorthern sky has provided so many radial-velocity data that orbits cannow be determined for many objects whose orbits were hitherto unknown orelse insecure or actually erroneous. Elements are given for the orbitsof 30 such objects, thereby more than doubling the number ofcomposite-spectrum binaries with known orbits.
| Visual multiples. VIII - 1000 MK types
A total of 1000 new classifications are given for stars brighter than B= 8.0 mag in the Aitken double star catalog. The classificationssupplement 865 classifications obtained in 1981 and 1984. Among thenewly discovered stars are 12 new Ap stars, eight Lambda Bootis stars,one Ba II star, and 60 Am stars. A detailed list of the newclassifications is given.
| Measurements of binary stars performed at Nice (Second series)
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1984A&AS...57..467M&db_key=AST
| Multicolor photometry of metallic-line stars. III. A photometric catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974RMxAA...1..175M&db_key=AST
| Spectral Classification of the Late Component of Stars with Composite Spectra
Not Available
| Peculiar and Metallic-Line a - Stars in a Galactic Zone.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1959ApJ...129...88S&db_key=AST
| M-Type Stars in NGC 7419.
Abstract image available at:http://adsabs.harvard.edu/abs/1955ApJ...121..637B
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| Takýmyýldýz: | Kral-Sefe |
| Sað Açýklýk: | 22h52m45.80s |
| Yükselim: | +60°54'58.6" |
| Görünürdeki Parlaklýk: | 7.574 |
| Uzaklýk: | 257.069 parsek |
| özdevim Sað Açýklýk: | -6.2 |
| özdevim Yükselim: | -12 |
| B-T magnitude: | 8.211 |
| V-T magnitude: | 7.627 |
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