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The Status of ROSAT X-ray Active Young Stars toward Taurus-Auriga
We present an astrometric study of the candidates of T Tauri stars (TTS)and non-TTS X-ray sources around Tau-Aur, based on the HipparcosCatalogue and the ACT Reference Catalogue. The ROSAT selected X-raysources are found to be a mixed population. A few of them areassociated with the Tau-Aur or Orion Star Forming Regions (SFR). Some,with distances similar to that of Tau-Aur but with discrepant propermotions, are probable or sure Pleiades super-cluster members or otherlate type young active stars with unresolved nature, more likely tooriginate in rapidly moving cloudlets, or else having originated fromdifferent sites other than Tau-Aur and moved to the present locations. Agood many of the non-TTS X-ray sources are considered as Hyades clustermembers. Some TTS candidates could be foreground pre-main sequencestars or actually young dwarfs not yet depleted of their Lithium. Underthe hypothesis that the sources we studied are representative of theROSAT selected TTS candidates discovered in the outskirts of the Tau-Aurregion, we conclude that only up to one third of the weak-line TTScandidates could be expected to be physically associated with theTau-Aur association. Along with the parallax and proper motion analysisof the non-TTS X-ray sources around the Tau-Aur SFR, our result suggeststhat the vast majority of the young active X-ray sources within anangular diameter of about 30 ° of the Tau-Aur SFR, belong to fourmain subgroups that are spatially separate.
| Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution
The kinematics of 237 chromospherically active binaries (CABs) werestudied. The sample is heterogeneous with different orbits andphysically different components from F to M spectral-type main-sequencestars to G and K giants and supergiants. The computed U, V, W spacevelocities indicate that the sample is also heterogeneous in velocityspace. That is, both kinematically younger and older systems exist amongthe non-evolved main sequence and the evolved binaries containing giantsand subgiants. The kinematically young (0.95 Gyr) subsample (N= 95),which is formed according to the kinematical criteria of moving groups,was compared with the rest (N= 142) of the sample (3.86 Gyr) toinvestigate any observational clues of binary evolution. Comparing theorbital period histograms between the younger and older subsamples,evidence was found supporting the finding of Demircan that the CABs losemass (and angular momentum) and evolve towards shorter orbital periods.The evidence of mass loss is noticeable on the histograms of the totalmass (Mh+Mc), which is compared between theyounger (only N= 53 systems available) and older subsamples (only N= 66systems available). The orbital period decrease during binary evolutionis found to be clearly indicated by the kinematical ages of 6.69, 5.19and 3.02 Gyr which were found in the subsamples according to the periodranges of logP<= 0.8, 0.8 < logP<= 1.7 and 1.7 < logP<=3, respectively, among the binaries in the older subsample.
| Reprocessing the Hipparcos Intermediate Astrometric Data of spectroscopic binaries. II. Systems with a giant component
By reanalyzing the Hipparcos Intermediate Astrometric Data of a largesample of spectroscopic binaries containing a giant, we obtain a sampleof 29 systems fulfilling a carefully derived set of constraints andhence for which we can derive an accurate orbital solution. Of these,one is a double-lined spectroscopic binary and six were not listed inthe DMSA/O section of the catalogue. Using our solutions, we derive themasses of the components in these systems and statistically analyzethem. We also briefly discuss each system individually.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997) and on data collected with theSimbad database.
| The Rotation of Binary Systems with Evolved Components
In the present study we analyze the behavior of the rotational velocity,vsini, for a large sample of 134 spectroscopic binary systems with agiant star component of luminosity class III, along the spectral regionfrom middle F to middle K. The distribution of vsini as a function ofcolor index B-V seems to follow the same behavior as their singlecounterparts, with a sudden decline around G0 III. Blueward of thisspectral type, namely, for binary systems with a giant F-type component,one sees a trend for a large spread in the rotational velocities, from afew to at least 40 km s-1. Along the G and K spectral regionsthere are a considerable number of binary systems with moderate tomoderately high rotation rates. This reflects the effects ofsynchronization between rotation and orbital motions. These rotatorshave orbital periods shorter than about 250 days and circular or nearlycircular orbits. Except for these synchronized systems, the largemajority of binary systems with a giant component of spectral type laterthan G0 III are composed of slow rotators.
| A catalog of rotational and radial velocities for evolved stars
Rotational and radial velocities have been measured for about 2000evolved stars of luminosity classes IV, III, II and Ib covering thespectral region F, G and K. The survey was carried out with the CORAVELspectrometer. The precision for the radial velocities is better than0.30 km s-1, whereas for the rotational velocity measurementsthe uncertainties are typically 1.0 km s-1 for subgiants andgiants and 2.0 km s-1 for class II giants and Ib supergiants.These data will add constraints to studies of the rotational behaviourof evolved stars as well as solid informations concerning the presenceof external rotational brakes, tidal interactions in evolved binarysystems and on the link between rotation, chemical abundance and stellaractivity. In this paper we present the rotational velocity v sin i andthe mean radial velocity for the stars of luminosity classes IV, III andII. Based on observations collected at the Haute--Provence Observatory,Saint--Michel, France and at the European Southern Observatory, LaSilla, Chile. Table \ref{tab5} also available in electronic form at CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| On X-Ray Variability in Active Binary Stars
We have compared the X-ray emissions of active binary stars observed atvarious epochs by the Einstein and ROSAT satellites in order toinvestigate the nature of their X-ray variability. The primary aim ofthis work is to determine whether or not active binaries exhibitlong-term variations in X-ray emission, perhaps analogous to theobserved cyclic behavior of solar magnetic activity. We find that, whilethe mean level of emission of the sample remains steady, comparison ofdifferent ROSAT observations of the same stars shows significantvariation on timescales <~2 yr, with an ``effective variability''ΔI/I=0.32+/-0.04, where I and ΔI represent the mean emissionand variation from the mean emission, respectively. A comparison of theROSAT All-Sky Survey and later pointed observations with earlierobservations of the same stars carried out with Einstein yields onlymarginal evidence for a larger variation (ΔI/I=0.38+/-0.04 forEinstein vs. ROSAT All-Sky Survey and 0.46+/-0.05 for Einstein vs. ROSATpointed) at these longer timescales (~10 yr), thus indicating thepossible presence of a long-term component to the variability. Whetheror not this long-term component is due to the presence of cyclicvariability cannot be decided on the basis of existing data. However,assuming that this component is analogous to the observed cyclicvariability of the Sun, we find that the relative magnitude of thecyclic component in the ROSAT passband can, at most, be a factor of 4,i.e., I_cyc/I_min<4. This is to be compared with the correspondingbut significantly higher solar value of ~10-10^2 derived from GOES,Yohkoh, and Solrad data. These results are consistent with thesuggestions of earlier studies that a turbulent or distributive dynamomight be responsible for the observed magnetic activity on the mostactive, rapidly rotating stars.
| Ten CORAVEL spectroscopic binary orbits of evolved stars
On the basis of Coravel observations, we present orbital parameters for10 spectroscopic-binary systems including an evolved star, namely HD13530, HD 28591, HD 47415, HD 78414, HD 123999, HD 153751, HD 174881, HD179094, HD 212280 and HD 217188. The most significant result is relatedto HD 13530, for which we have found an orbital period of 1575.48+/-1.63days and an eccentricity of 0.8815. Such an eccentricity value is thelargest one known up to date for a single-lined spectroscopic binarywith a giant component. The other spectroscopic orbits described in thispaper principally confirm with independent data previously obtainedorbital solutions except HD 179094 for which the double-lined status wasstill unknown. Based on observations collected at the Haute-ProvenceObservatory, Saint-Michel, France and at ESO, La Silla, Chile.
| Newly discovered candidate weak-line T Tauri stars in the surrounding area of the Taurus-Auriga region
We present results of an extensive search for weak-line T Tauri stars(WTTS) in the outskirts of the Taurus-Auriga molecular cloud on thebasis of the ROSAT All-Sky Survey Bright Source Catalog. Our surveyedregion extends from 2() h40() m to 5() h40() m in right ascension andfrom 10(deg) to 40(deg) in declination, with the central part ofTaurus-Auriga (4() h
| The age-mass relation for chromospherically active binaries. III. Lithium depletion in giant components
We present a study of the lithium abundances of a sample of evolvedcomponents of Chromospherically Active Binary Systems. We show that asignificant part of them have lithium excesses, independently of theirmass and evolutionary stage. Therefore, it can be concluded that Liabundance does not depend on age for giant components of CABS. Theseoverabundances appear to be closely related to the stellar rotation, andwe interpret them as a consequence of the transfer of angular momentumfrom the orbit to the rotation as the stars evolve in and off the MainSequence, in a similar way as it happens in the dwarf components of thesame systems and in the Tidally Locked Binaries belonging to the Hyadesand M67. Based on observations collected with the 2.2\,m telescope ofthe German-Spanish Observatorio de Calar Alto (Almeria, Spain), and withthe 2.56\,m Nordic Optical Telescope in the Spanish Observatorio delRoque de los Muchachos of the Instituto de Astrof\'\i sica de Canarias(La Palma, Spain)
| Mesures de vitesses radiales. VIII. Accompagnement AU sol DU programme d'observation DU satellite HIPPARCOS
We publish 1879 radial velocities of stars distributed in 105 fields of4^{\circ} \times 4^{\circ}. We continue the PPO series \cite[(Fehrenbachet al. 1987;]{Feh87} \cite[Duflot et al. 1990, 1992 and 1995),]{Du90}using the Fehrenbach objective prism method. Table 1 only available inelectronic form at CDS via to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Rotational Velocities of Late-Type Stars
A calibration based on the results of Gray has been used to determineprojected rotational velocities for 133 bright stars with spectral typesof F, G, or K, most of which appear in {\it The Bright Star Catalogue}.The vast majority have {\it v} sin {\it i} $\leq$ 10 km s$^{-1}$ and,thus, are slow rotators. With the new calibration, projected rotationalvelocities have been determined for a sample of 111 late-type stars,most of which are chromospherically active. Some of the stars have hadtheir rotational velocities measured for the first time. (SECTION:Stars)
| A Search for Optical Flares in Chromospherically Active Stars
We have surveyed four years of archival UBV photometry of 69chromospherically active stars obtained with the Phoenix-10 automaticphotoelectric telescope in search of optical flares on these stars. Wedemonstrate taht, while flares can be detected in these data, the numberof events observed on evolved stars remains very small. Flares werefound only on UX Arietis, II Pegasi, and AR Piscium. (SECTION: Stars)
| Are the Rotational Axes Perpendicular to the Orbital Planes in the Binary Systems? II. Synchronous Long-Period RS CVn Stars
Inclinations of the rotational axes, irot, are determined for37 synchronous long-period RS CVn binaries by combining v sin imeasurements with rotational period information. These inclinations arethen compared with the orbital inclinations of the systems,iorb, to test the alignment between the equatorial andorbital planes. Contrary to the asynchronous RS CVn systems (see PaperI), in all 37 cases irot is equal or nearly equal toiorb, and the assumption about coplanarity of theirequatorial and orbital planes is justified.
| Lithium in Rs-Canum Binaries and Related Chromospherically Active Stars - Part Three - Northern Rs-Canum Systems
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994A&A...283..893R&db_key=AST
| The active dynamo stars: RS CVn, BY Dra, FK Com, Algol, W UMa, and T Tau
Not Available
| A catalog of chromospherically active binary stars (second edition)
The catalog contains 206 spectroscopic binary systems with at least onelate-type component that shows Ca II H and K emission in its spectrum.These systems include the classical RS CVn binaries and BY Dra binaries.The catalog summarizes information on the photometric, spectroscopic,orbital, and physical properties of the systems as well as space motionsand positions. Up to 42 'parameters' for each stellar system are listedfollowed by the appropriate reference to direct interested colleagues tothe original papers. A comprehensive selection of further informationfor each star is given in the individual notes. In addition, the catalogcontains a candidate list of 138 stars that have similar characteristicsbut are not definitely known binaries or have not had Ca II H and Kemission observed.
| Observations of the CA II infrared triplet in chromospherically active single and binary stars
Spectroscopic observations of the Ca II infrared triplet (8498, 8542,8662 A) have been obtained for 45 stars which are known or suspected tobe chromospherically active. The sample includes both single and binarystars of spectral types from F2 to M5 spanning luminosity classes III,IV, and V. Several different types of activity diagnostics weremeasured, and their relative merits are discussed. Dependence ofchromospheric emission upon rotation period, luminosity, temperature,and duplicity are analyzed. Synchronous binaries show a slight trend ofincreased emission with decreasing period while the asynchronousbinaries show abnormally high activity levels for their rotationperiods. Several stars exhibit rotationally modulated emission which isanticorrelated with the stellar brightness. Finally, estimates ofchromospheric energy losses are presented with the result that the totalloss in the infrared triplet is about twice that of the H and K lines.
| Statistical Analysis of a Sample of Spectroscopic Binaries Containing Late Type Giants
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993A&A...271..125B&db_key=AST
| Lithium and rapid rotation in chromospherically active single giants
The rotational velocities presently obtained via spectroscopicobservations of a group of moderately rapidly rotating, chomosphericallyactive single giants indicate that Gray's (1989) rotostat hypothesisrequires modification. Their rapid rotation appears to be due to high Liabundances, and results in increased chromospheric activity. A scenariois projected in which the surface convection zone reaches the rapidlyrotating core just as a star begins its first ascent of the giantbranch, and dredges both high angular momentum material and freshlysynthesized Li to the surface.
| Radio continuum and X-ray properties of the coronae of RS Canum Venaticorum and related active binary systems
Data from circular polarization measurements are reported which yieldradio-continuum and X-ray characterizations of the coronae of activebinaries including RS CVn. The circular polarization measurements aretaken at 6 cm for 28 binary systems detected at flux densities of morethan 0.7 mJy, and the data are examined in conjunction with those byDrake et al. (1989). Optical positions are derived for 8 RS CVn objects,three previous detections are confirmed, and seven sources are shown tohave circular polarization at levels of 2-13 percent. A total of 49X-ray sources are confirmed in a total of 190 positions, and thecorrelation between X-ray and radio emissions is analyzed. Noobservational evidence exists to support the notion that radio and X-rayemissions are due to nonthermal electrons, and the data provide evidencefor and against thermal gyrosynchrotron radio emission.
| Synoptic APT Photometry of the RS CVn Binary HD 28591
HD 28591 is a single-lined, non-eclipsing RS CVn binary which exhibitsphotometric variations indicative of starspot activity. We report on Band V observations obtained over the period 1988-1992 with thePhoenix-10 Automatic Photoelectric Telescope sited on Mt. Hopkins, AZ.The system exhibits a variable distortion wave with amplitudes rangingfrom 0.04 to 0.07 magnitudes in V as well as a variable mean lightlevel. A Scargle periodogram analysis of the entire dataset shows ahighly significant peak at a period of 10.650 days. As this is exactlyhalf the reported orbital period of 21.3 days, this casts doubt on itsvalidity as the rotational period of the primary. Inspection of thedifferential magnitudes plotted against J. D. as well as light curvesphased with both periods leaves little doubt that the star issynchronously rotating but with a light curve that shows two, oftenunequal, maxima per orbit. We have modelled the B and V datasimultaneously using the formalism of Budding (1977). This analysisindicates that two distinct spot groups, widely separated in longitude,are needed during all seasons to accurately model the light curves. Theresults for the individual years show evolution over time of both thespot sizes and longitudes. The measurement of the total spotted areas inthese seasons ranges from approximately 0.017 to 0.034 of the totalsurface area and shows some preliminary indications of a starspot cyclein HD 28591.
| Line profile asymmetries in chromospherically active stars
A powerful, new probe of chromospheric activity, cross-correlation, hasbeen developed and applied to a variety of stars. In this particularapplication, an entire CCD spectrum of an active star is correlated withthe spectrum of a narrow-line, inactive star of similar spectral typeand luminosity class. Using a number of strong lines in this mannerenables the detection of absorption profile asymmetries at moderateresolution (lambda/Delta lambda about 40,000) and S/N 150:1. Thistechnique has been applied to 14 systems mostly RS CVn's, with 10 notgreater than nu sin i not greater than 50 km/s and P not less than 7 d.Distortions were detected for the first time in five systems: Sigma Gem,IM Peg, GX Lib, UV Crb, and Zeta And. Detailed modeling, incorporatingboth spectral line profiles and broad-band photometry, is applied toSigma Gem. Profile asymmetries for this star are fitted by twohigh-latitude spots covering 5 percent of the stellar surface. Thederived spot temperature of 3400 K is lower than found in previousstudies. In addition, two well-known systems have been studied: HD199178 and V711 Tau. Polar spots are found on both.
| Kinematics and age of RS Canum Venaticorum and by Draconis stars
Space velocities of 146 chromospherically active binary stars have beencalculated. Containing F-M spectral types on the main sequence togetherwith G and K giants and subgiants, this very heterogeneous sample hasbeen divided into groups in order to segregate stars which have similarkinematics and ages. After many trials for different criteria, thesample was divided into five groups - two groups for giants, two groupsfor main-sequence systems, and one group for main-sequence systems.Kinematics of subgiants implies a stellar age of about 2-3 Gyr. Youngand old groups of giants and main-sequence systems could becharacterized by a kinematical age of about 1 Gyr and more than 5 Gyr,respectively. These ages are estimated approximately according to spacevelocity distributions and dispersions in velocity space in each group.Inferred ages for the groups above agrees with circulation, rotationactivity relation, and stellar evolution theories.
| Chromospheric CA II H and K and H-alpha emission in single and binary stars of spectral types F6-M2
New observations of the Ca II H and K and H-epsilon region and/or theBalmer H-alpha line are presented for 100 mostly very active stars butalso for weak or inactive stars with suspected activity. Correlationsbetween chromospheric activity at Ca II H and K and H-alpha andeffective surface temperature and rotation are identified, and severalnew stars with chromospheric Ca II H and K emission are discovered. Nosingle activity-rotation relation can be derived for all luminosityclasses, and there is clear evidence that evolved stars are generallymore active than main-sequence stars of the same rotation period. Binarywithin the evolved stars appears to play no role, while main-sequencebinary stars show generally higher levels of activity than their singlecounterparts. Chromospheric emission in the Ca II H and K lines dependson surface temperature in that flux declines with cooler temperature.
| Photometric variability in chromospherically active stars. III - The binary stars
Differential UBV photometry of 49 late-type chromospherically activebinary stars has been obtained. A total of 12,353 differential UBVmagnitudes have been acquired and are used to determine seasonalphotometric periods, amplitudes, mean brightnesses, maximum spotamplitudes, 'unspotted' differential magnitudes, and times of minimumlight. Standard Fourier techniques are used to investigate the cause ofthe light variability. Eight stars are found which exhibit lightvariations due not to spot activity but rather to ellipticity and/orreflection effect. Others show combinations of all three effects. Someof the systems also show substantial differences between theirrotational and orbital period.
| A catalog of chromospherically active binary stars
A catalog of 168 chromospherically active binary stars is presented,including the class of RS CVn, BY Dra binaries, and other binaries whichshow strong Ca II H and K emission in their spectra. The catalogcontains information on the photometric, spectroscopic, orbital, andphysical properties of the systems as well as the space motions andpositions. Summarized in a candidate list are in additional 37 starshaving similar characteristics but which are not definitely knownbinaries or have not had H and K emission observed. The catalog containsstars in both the northern and the southern sky.
| The 68th Name-List of Variable Stars
Not Available
| APT's - Automatic photoelectric telescopes
In an automatic photoelectric telescope (APT), the photometricinstrument with which measurements are made also undertakes theidentification and centering of the stars to be observed. Amicrocomputer operates both the photometer and telescope, and inaddition decides the time and order of observations. APTs are noted toexcell in the detection of variable stars with properties, such as longperiods, which could easily be missed during the shorter observationruns to which human astronomers are accustomed. A detailed account isgiven of an APT's typical operating cycle.
| Automatic Photoelectric Telescope: Second and Third Quarter 1984 Observations
Not Available
| Automatic Photoelectric Telescope: First Quarter 1984 Observations
Not Available
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| Csillagkép: | Perszeusz |
| Rektaszcenzió: | 04h31m56.95s |
| Deklináció: | +36°44'33.7" |
| Vizuális fényesség: | 6.349 |
| Távolság: | 118.064 parszek |
| RA sajátmozgás: | 4.8 |
| Dec sajátmozgás: | -67.5 |
| B-T magnitude: | 7.734 |
| V-T magnitude: | 6.464 |
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