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A catalogue of chromospherically active binary stars (third edition)
The catalogue of chromospherically active binaries (CABs) has beenrevised and updated. With 203 new identifications, the number of CABstars is increased to 409. The catalogue is available in electronicformat where each system has a number of lines (suborders) with a uniqueorder number. The columns contain data of limited numbers of selectedcross references, comments to explain peculiarities and the position ofthe binarity in case it belongs to a multiple system, classicalidentifications (RS Canum Venaticorum, BY Draconis), brightness andcolours, photometric and spectroscopic data, a description of emissionfeatures (CaII H and K, Hα, ultraviolet, infrared),X-ray luminosity, radio flux, physical quantities and orbitalinformation, where each basic entry is referenced so users can go to theoriginal sources.
| Dynamical evolution of active detached binaries on the logJo-logM diagram and contact binary formation
Orbital angular momentum (OAM, Jo), systemic mass (M) andorbital period (P) distributions of chromospherically active binaries(CAB) and W Ursae Majoris (W UMa) systems were investigated. Thediagrams of and logJo-logM were formed from 119 CAB and 102 WUMa stars. The logJo-logM diagram is found to be mostmeaningful in demonstrating dynamical evolution of binary star orbits. Aslightly curved borderline (contact border) separating the detached andthe contact systems was discovered on the logJo-logM diagram.Since the orbital size (a) and period (P) of binaries are determined bytheir current Jo, M and mass ratio, q, the rates of OAM loss(dlogJo/dt) and mass loss (dlogM/dt) are primary parametersto determine the direction and the speed of the dynamical evolution. Adetached system becomes a contact system if its own dynamical evolutionenables it to pass the contact border on the logJo-logMdiagram. The evolution of q for a mass-losing detached system is unknownunless the mass-loss rate for each component is known. Assuming q isconstant in the first approximation and using the mean decreasing ratesof Jo and M from the kinematical ages of CAB stars, it hasbeen predicted that 11, 23 and 39 per cent of current CAB stars wouldtransform to W UMa systems if their nuclear evolution permits them tolive 2, 4 and 6 Gyr, respectively.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Mass loss and orbital period decrease in detached chromospherically active binaries
The secular evolution of the orbital angular momentum (OAM), thesystemic mass (M=M1+M2) and the orbital period of114 chromospherically active binaries (CABs) were investigated afterdetermining the kinematical ages of the subsamples which were setaccording to OAM bins. OAMs, systemic masses and orbital periods wereshown to be decreasing by the kinematical ages. The first-orderdecreasing rates of OAM, systemic mass and orbital period have beendetermined as per systemic OAM, per systemic mass and per orbitalperiod, respectively, from the kinematical ages. The ratio of d logJ/dlogM= 2.68, which were derived from the kinematics of the presentsample, implies that there must be a mechanism which amplifies theangular momentum loss (AML) times in comparison to isotropic AML ofhypothetical isotropic wind from the components. It has been shown thatsimple isotropic mass loss from the surface of a component or bothcomponents would increase the orbital period.
| The photospheric abundances of active binaries. III. Abundance peculiarities at high activity levels
We report the determination from high-resolution spectra of theatmospheric parameters and abundances of 13 chemical species (amongwhich lithium) in 8 single-lined active binaries. These data arecombined with our previous results for 6 other RS CVn systems to examinea possible relationship between the photospheric abundance patterns andthe stellar activity level. The stars analyzed are generally found toexhibit peculiar abundance ratios compared to inactive, Galactic diskstars of similar metallicities. We argue that this behaviour is unlikelyto be an artefact of errors in the determination of the atmosphericparameters or non-standard mixing processes along the red giant branch,but diagnoses instead the combined action of various physical processesrelated to activity. The most promising candidates are cool spot groupscovering a very substantial fraction of the stellar photosphere or NLTEeffects arising from nonthermal excitation. However, we cannot excludethe possibility that more general shortcomings in our understanding ofK-type stars (e.g. inadequacies in the atmospheric models) also play asignificant role. Lastly, we call attention to the unreliability of the(V-R) and (V-I) colour indices as temperature indicators inchromospherically active stars.Based on observations collected at the European Southern Observatory,Chile (Proposals 64.L-0249 and 071.D-0260).Table A.1 is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/426/1007
| SB9: The ninth catalogue of spectroscopic binary orbits
The Ninth Catalogue of Spectroscopic Binary Orbits(http://sb9.astro.ulb.ac.be) continues the series of compilations ofspectroscopic orbits carried out over the past 35 years by Batten andcollaborators. As of 2004 May 1st, the new Catalogue holds orbits for2386 systems. Some essential differences between this catalogue and itspredecessors are outlined and three straightforward applications arepresented: (1) completeness assessment: period distribution of SB1s andSB2s; (2) shortest periods across the H-R diagram; (3)period-eccentricity relation.
| On the determination of oxygen abundances in chromospherically active stars
We discuss oxygen abundances derived from [O I] λ6300s and the OI triplet in stars spanning a wide range in chromospheric activitylevel, and show that these two indicators yield increasingly discrepantresults with higher chromospheric/coronal activity measures. While theforbidden and permitted lines give fairly consistent results forsolar-type disk dwarfs, spuriously high O I triplet abundances areobserved in young Hyades and Pleiades stars, as well as in individualcomponents of RS CVn binaries (up to 1.8 dex). The distinct behaviour ofthe [O I]-based abundances which consistently remain near-solar suggeststhat this phenomenon mostly results from large departures from LTEaffecting the O I triplet at high activity level that are currentlyunaccounted for, but also possibly from a failure to adequately modelthe atmospheres of K-type stars. These results suggest that some cautionshould be exercised when interpreting oxygen abundances in activebinaries or young open cluster stars.Based on observations collected at the European Southern Observatory,Chile (Proposals 64.L-0249 and 071.D-0260).Table \ref{tab_data} is only available in electronic form athttp://www.edpsciences.org
| 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.
| The photospheric abundances of active binaries. II. Atmospheric parameters and abundance patterns for 6 single-lined RS CVn systems
Photospheric parameters and abundances are presented for a sample ofsingle-lined chromospherically active binaries from a differential LTEanalysis of high-resolution spectra. Abundances have been derived for 13chemical species, including several key elements such as Li, Mg, and Ca.Two methods have been used. The effective temperatures, surfacegravities and microturbulent velocities were first derived from a fullyself-consistent analysis of the spectra, whereby the temperature isdetermined from the excitation equilibrium of the Fe I lines. The secondapproach relies on temperatures derived from the (B-V) colour index.These two methods give broadly consistent results for the stars in oursample, suggesting that the neutral iron lines are formed underconditions close to LTE. We discuss the reliability in the context ofchromospherically active stars of various colour indices used astemperature indicators, and conclude that the (V-R) and (V-I) coloursare likely to be significantly affected by activity processes.Irrespective of the method used, our results indicate that the X-rayactive binaries studied are not as metal poor as previously claimed, butare at most mildly iron-depleted relative to the Sun (-0.41protect <~[Fe/H]protect la +0.11). A significant overabundance of several chemicalspecies is observed (e.g., the alpha -synthezised elements). Theseabundance patterns are discussed in relation to stellar activity.Based on observations collected at ESO (La Silla, Chile).Table A.1 is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/412/495
| The photospheric abundances of active binaries. I. Detailed analysis of HD 113816 (IS Vir) and HD 119285 (V851 Cen)
The high-resolution optical spectra of the two X-ray active binaries RSCVn stars HD 113816 (IS Vir) and HD 119285 (V851 Cen) are analysed andtheir Na, Mg, Al, Si, Ca, Sc, Ti, Co and Ni contents determined, in theframework of a larger program of chemical analysis of RS CVn stellaratmosphere. The analysis of IS Vir and V851 Cen is performed with threedifferent LTE methods. In the first one, abundances are derived for alarge set of transitions (among which 28 Fe I lines, spanning a broadinterval in excitation potential and equivalent width, and 6 Fe IItransitions) using measured equivalent widths and Kurucz LTE modelatmospheres as input for the MOOG software package. The inputatmospheric parameters and abundances are iteratively modified until (i)the Fe I abundances exhibit no trend with excitation potential orequivalent width, (ii) Fe I and Fe II average abundances are the sameand (iii) Fe and Alpha elements average abundances are consistent withthe input values. The second method follows a similar approach, but usesa restricted line list (without the Fe I ``low excitation potential''transitions) and relies on the B-V and V-I colour indices to determinethe temperature. The third method uses the same restricted line list asthe second method and relies on fitting the 6162 Å Ca I line wingprofiles to derive the surface gravity. The reliability of these methodsis investigated in the context of single line RS CVn stars. It is shownthat the V-I photometric index gives, on a broader sample of stars,significantly cooler estimates of the effective temperature than the B-Vindex. All approaches give results in good agreement with each other,except the V-I based method. The analysis of IS Vir and V851 Cen resultsin both cases in their primaries being giant stars of near-solarmetallicity. Their parameters as derived with the first method arerespectively T_eff = 4720 K, log g = 2.65, [Fe/H] = +0.04 and T_eff =4700 K, log g = 3.0 and [Fe/H] = -0.13. In the case of V851 Cen thederived iron content is significantly higher than a previousdetermination in the literature. Both stars exhibit relativeoverabundances of several elements (e.g. Ca) with respect to the solarmix. Table 2 is only available in electronic form athttp://www.edpsciences.org
| Chromospherically Active Stars. XXI. The Giant, Single-lined Binaries HD 89546 And HD 113816
We have obtained spectroscopy and photometry of the chromosphericallyactive, single-lined spectroscopic binaries HD 89546 and HD 113816. HD89546 has a circular orbit with a period of 21.3596 days. Its primaryhas a spectral type of G9 III and is somewhat metal-poor with[Fe/H]~-0.5. HD 113816 has an orbit with a period of 23.6546 and a loweccentricity of 0.022. Its mass function is extremely small, 0.0007Msolar, consistent with a very low inclination. The primaryis a slightly metal-poor K2 III. A decade or more of photometricmonitoring with an automatic telescope demonstrates that both systemsdisplay brightness variations due to rotational modulation of thevisibility of photospheric star spots, as well as light-curve changesresulting from the redistribution of star spots by differential rotationand long-term changes in the filling factor of the spots. We determinedrotation periods for each season when the observations were numerousenough. Our mean rotation periods of 21.3 and 24.1 days for HD 89546 andHD 113816, respectively, confirm that the giants in each system aresynchronously rotating. The orbital elements and properties of the giantcomponents of these two systems, including levels of surface magneticactivity, are quite similar. However, the two rotational inclinationsare rather different, 57° for HD 89546 and 13° for HD 113816.Thus the latter giant is seen nearly pole on. We analyzed the lightcurves for similarities and differences that result from viewing thesetwo systems from quite different inclinations.
| Multiwavelength optical observations of chromospherically active binary systems. III. High resolution echelle spectra from Ca ii H & K to Ca ii IRT
This is the third paper of a series aimed at studying the chromosphereof active binary systems using the information provided for severaloptical spectroscopic features. High resolution echelle spectraincluding all the optical chromospheric activity indicators from the Caii H & K to Ca ii IRT lines are analysed here for 16 systems. Thechromospheric contribution in these lines has been determined using thespectral subtraction technique. Very broad wings have been found in thesubtracted Hα profile of the very active star HU Vir. Theseprofiles are well matched using a two-component Gaussian fit (narrow andbroad) and the broad component can be interpreted as arising frommicroflaring. Red-shifted absorption features in the Hα line havebeen detected in several systems and excess emission in the blue wing ofFG UMa was also detected. These features indicate that several dynamicalprocesses, or a combination of them, may be involved. Using theE_Hα /E_Hβ ratio as a diagnostic we have detectedprominence-like extended material viewed off the limb in many stars ofthe sample, and prominences viewed against the disk at some orbitalphases in the dwarfs OU Gem and BF Lyn. The He i D3 line hasbeen detected as an absorption feature in mainly all the giants of thesample. Total filling-in of the He i D3, probably due tomicroflaring activity, is observed in HU Vir. Self-absorption with redasymmetry is detected in the Ca ii H & K lines of the giants 12 Cam,FG UMa and BM CVn. All the stars analysed show clear filled-in Ca ii IRTlines or even notable emission reversal. The small values of theE_8542/E_8498 ratio we have found indicate Ca ii IRT emission arisesfrom plage-like regions. Orbital phase modulation of the chromosphericemission has been detected in some systems, in the case of HU Virevidence of an active longitude area has been found. Based onobservations made with the Isaac Newton Telescope (INT) operated on theisland of La Palma by the Isaac Newton Group in the Spanish Observatoriodel Roque de Los Muchachos of the Instituto de Astrofísica deCanarias, and with the Nordic Optical Telescope (NOT), operated on theisland of La Palma jointly by Denmark, Finland, Iceland, Norway andSweden, in the Spanish Observatorio del Roque de los Muchachos of theInstituto de Astrofísica de Canarias. Tables 3, 5, 6, 7 also atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| 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
| 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.
| 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)
| Starspot photometry with robotic telescopes: Continuous UBV and V(RI)_C photometry of 23 stars in 1991-1996
We report on the progress of our ongoing photometric monitoring programof spotted late-type stars with automatic photoelectric telescopes(APTs) on Mt. Hopkins in Arizona and on Mt. Etna in Sicily. We present9,250 differential UBV and/or V(RI)_C observations for altogether 23chromospherically active stars, singles and binaries, pre main sequenceand post main sequence, taken between 1991 and 1996. The variabilitymechanism of our target stars is mostly rotational modulation by anasymmetrically spotted stellar surface. Therefore, precise rotationalperiods and their seasonal variations are determined using baselinesbetween 3 years for HD 129333 to 34 years for V410 Tauri. We report thelargest V light-curve amplitude of any spotted star observed to date:0.65" for V410 Tau in 1994-95. Long-term variations of the overall lightlevels of our target stars are sometimes of similar amplitude as therotational modulation itself and are most likely caused by an analog ofthe solar 11-year spot cycle but mostly without a well-definedperiodicity. For some of our target stars (HD 12545, HD 17433, EI Eri,V410 Tau, LQ Hya, and HD 106225) we estimate a probable cycle period. Acomplete light curve of the semi-regular S-type giant HR Pegasii ispresented. All data are available via the WorldWideWeb. Data areavailable at the CDS via anonymous ftp.
| 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)
| The 73rd Name-List of Variable Stars
Not Available
| EUV Emission from RS Canum Venaticorum binaries.
We performed a study of 104 RS CVn systems in the extreme ultraviolet(EUV) using the all-sky survey data obtained by the Extreme UltravioletExplorer (EUVE). The present sample includes several new RS CVndetections; 11 more than in the published EUVE catalogs, and 8 more thanin the ROSAT Wide Field Camera catalog. The ratio of detections tonon-detections remained constant throughout the sky, implying that ourdetections are not limited by the exposure time but are most likelylimited by absorption from the interstellar medium. A general trend ofincreasing Lex/B (50-180Å) flux with decreasing rotational periodis clear. The dwarf systems exhibit a leveling-off for the fasterrotators. In contrast, the evolved systems exhibit no such effect. Forthe RS CVn systems the losses in the EUV represent a smaller fraction ofthe coronal radiative losses, as compared to active late-type dwarfs.
| The behaviour of the excess CA II H and K and Hɛ emissions in chromospherically active binaries.
In this work we analyze the behaviour of the excess Ca II H and K andHɛ emissions in a sample of 73 chromospherically active binarysystems (RS CVn and BY Dra classes), of different activity levels andluminosity classes. This sample includes the 53 stars analyzed byFernandez-Figueroa et al. (1994) and the observations of 28 systemsdescribed by Montes et al. (1995c). By using the spectral subtractiontechnique (subtraction of a synthesized stellar spectrum constructedfrom reference stars of spectral type and luminosity class similar tothose of the binary star components) we obtain the active-chromospherecontribution to the Ca II H and K lines in these 73 systems. We havedetermined the excess Ca II H and K emission equivalent widths andconverted them into surface fluxes. The emissions arising from eachcomponent were obtained when it was possible to deblend bothcontributions. We have found that the components of active binaries aregenerally stronger emitters than single active stars for a giveneffective temperature and rotation rate. A slight decline of the excessCa II H and K emissions towards longer rotation periods, P_rot_, andlarger Rossby numbers, R_0_, is found. When we use R_0_ instead ofP_rot_ the scatter is reduced and a saturation at R_0_=~0.3 is observed.A good correlation between the excess Ca II K and Hɛchromospheric emission fluxes has been found. The correlations obtainedbetween the excess Ca II K emission and other activity indicators, (C IVin the transition region, and X-rays in the corona) indicate that theexponents of the power-law relations increase with the formationtemperature of the spectral features.
| A new H-alpha survey of chromospherically active binaries.
Not Available
| The emission of the RS CVn binaries in the IRAS passbands.
In the literature, there is an ambiguity pertaining to the existence ofa far-IR excess in RS CVn systems. In the current paper we undertook astudy of the behaviour of 103 such systems in the IRAS passbands. Wefound 72 acceptable detections in the 12μm band, and 40 in the25μm band (50% more than the IRAS Point Source Catalog). Although ourfindings may be interpreted as indicating towards the existence of anexcess beyond 12μm for some systems, the evidence is not conclusivein all but two cases. These are systems GX Lib and HR 7428, with Capellabeing the only system where the IRAS fluxes in all four bands originatefrom the stellar photosphere. Given the accuracy of the data we did notfind 12μm excess for any system. We argue that the IRAS data alonecannot settle the issue, as their uncertainty is, in many cases, higherthan what the Signal-to-Noise ratio of each observation implies.Furthermore, at the higher wavelength bands the IRAS angular resolutiondrops from 0.5' at 12μm to 2' at 100μm and the background becomesvery complex, so one cannot be certain about the origin of the observedflux. The existence of IR excess in the RS CVn stars is important as faras the evolutionary scenarios for these systems are concerned. Futuremissions such as the Infrared Space Observatory will return moresensitive and accurate measurements and the ambiguity can be removed.The fluxes we quote will be helpful when planning these futureobservations, as we provide more accurate photometry and for a largerselection of sources than the IRAS Point Source Catalog.
| An Automated Search for Variability in Chromospherically Active Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....110.2926H&db_key=AST
| Application of the spectral subtraction technique to the CA II H & K and Hɛ lines in a sample of chromospherically active binaries.
We present new spectroscopic observations in the Ca II H & K lineregion for a sample of 28 chromospherically active binary systems (RSCVn and BY Dra classes), with different activity levels. By using thespectral subtraction technique (subtraction of a synthesized stellarspectrum constructed from reference stars of similar spectral type andluminosity class) we obtain the active-chromosphere contribution to theCa II H & K lines and to the Hɛ line when it is present. Wehave compared the emission equivalent widths obtained with thistechnique with those obtained by reconstruction of the absorption lineprofile below the emission peak(s). The emissions arising from eachindividual star were obtained when it was possible to deblend thecontribution of both components. The Ca II line profiles correspondingto different seasons and orbital phases are analysed in order todetermine the contribution of each component and to study thechromospheric activity variations.
| Radio continuum emission from stars: a catalogue update.
An updated version of my catalogue of radio stars is presented. Somestatistics and availability are discussed.
| The Wilson-Bappu effect and other CA II H and K line parameters relationships in chromospherically active binaries
We present measurements of the emission core width W_0_ and thewavelength separation of the K_1_ dips, W_1_, of the Ca II H and Kemission lines observed on high-dispersion spectra of 28chromospherically active binary systems (RS CVn and BY Dra stars) and 18single active stars. We test the width-luminosity correlations (theWilson-Bappu (WB) effect, and (W_1_, M_V_)) in these very active starsand analyse the influence of the activity level (I_K_3__) and therotational broadening (Vsin i) in these correlations. We have found thatfor very active stars the emission widths, both W_0_ and W_1_, arelarger than expected from previously accepted width-luminosityrelations. The stars with strong emission intensities, I_K_3__, andlarge values of Vsin i seem to present larger values of W_0_ thanresulted from WB relation, the effect of the rotational velocity beingthe most remarkable. On the contrary, W_1_ is strongly influenced byI_K_3__ but the effect of the rotational broadening is lesser. We alsoanalyse the behaviour of the Ca II H and K line parameters in these veryactive stars in relation with less active stars and we found that theincrease of W_1_ and I_K_1__ with I_K_3__ presents a flattening for themost active stars which is different for each value of W_0_. Finally wealso find a Hɛ width-luminosity correlation in the stars of thesample in which this emission line is present.
| Chromospheric activity in G and K giants: the spectroscopic data base
I present high-resolution CCD spectra of CaII H and K emission lines of59 evolved stars of spectral type G and K and luminosity Class III,III-IV, and IV. This includes active stars like RS CVn binaries but alsoactive and inactive single stars. Most of the objects were observed forthe first time and several were discovered to be chromosphericallyactive. Spectra for ten stars of luminosity Class V are also given.
| 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
| Chromospheric activity in G and K giants and their rotation-activity relation
We obtained high-resolution CCD spectra of Ca II H and K emission linesof 59 evolved stars of spectral type G and K and luminosity class III,III-IV, and IV. Our sample includes active stars like RS CVn binariesbut also active and inactive single stars. Whenever possible wedetermine absolute emission line surface fluxes and use them,supplemented by previously published fluxes from high-resolutionspectra, to quantify the rotation-activity relation for evolved stars.We find that the Ca II surface fluxes from evolved stars scale linearlywith stellar rotational velocity and that the flux from the cooler starsdepends stronger upon rotation than the flux from the hotter stars, inagreement with previous findings for main-sequence stars. However, largescatter indicates that rotational velocity might not be the onlyrelevant parameter. We also present some evidence for the existence of a'basal' flux for evolved stars that scales approximately with the eightpower of the effective surface temperature.
| 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.
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Наблюдательные данные и астрометрия
| Созвездие: | Дева |
| Прямое восхождение: | 13h06m26.01s |
| Склонение: | -04°50'45.3" |
| Видимая звёздная величина: | 8.366 |
| Расстояние: | 300.3 парсек |
| Собственное движение RA: | -3.3 |
| Собственное движение Dec: | -18.9 |
| B-T magnitude: | 9.822 |
| V-T magnitude: | 8.487 |
Каталоги и обозначения:
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