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Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188
We have obtained spectroscopy and photometry of three chromosphericallyactive, single-lined spectroscopic binaries, HD 37824 (V1149 Ori), HD181809 (V4138 Sgr), and HD 217188 (AZ Psc). HD 37824 has a circularorbit with a period of 53.57 days. Its primary is a K0 III star, whilethe secondary is likely a G or K dwarf. HD 181809 has an orbit with aperiod of 13.04667 days and a low eccentricity of 0.040. The primary hasa spectral type of K0 III-IV, and its secondary is probably an M dwarf.The orbit of HD 217188 has a period of 47.1209 days and a moderatelyhigh eccentricity of 0.470. The spectral type of the primary is K0 III,while the secondary is likely an M dwarf. All three systems areestimated to have near solar iron abundances. Photometric observationsspanning 15-16 years for all three stars yield mean photometric periodsof 53.12, 59.85, and 90.89 days for HD 37824, HD 181809, and HD 217188,respectively. Thus, HD 37824 is rotating synchronously with the orbitalperiod, while HD 181809 and HD 217188 are both rotating considerablyslower than synchronously. All three stars show long-term variations inmean brightness and photometric amplitude, but no correlations areobserved between the seasonal mean brightness, photometric amplitude,and seasonal photometric period in any of the stars. No clear evidencefor long-term periodic variations in any of these parameters is present.The circular orbit of HD 37824 and the synchronous rotation of its Kgiant argue that the star is in the core helium-burning phase of itsevolution. The giant components of HD 181809 and HD 217188 areasynchronous rotators, and both systems have eccentric orbits. Thus,those two stars are likely first-ascent giants.
| 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.
| Effect of chromospheric activity on the mean colours of late-type stars. II. Is (B-V)0 also affected?
We confirm the existence of an ``excess'' in the mean dereddened(U-B)0 colour of active single-lined spectroscopic giantsover quiescent stars of the same spectral type and find evidence forthis ``excess'' in (B-V)0, although at a lower scale, whenplotted against (R-I)0. This result suggests that the use of(B-V)0 calibrations to determine fundamental parameters orspectral types for late-type active stars should be taken with caution.Since magnetic activity is definitely involved, these and similarcalibrations using (U-B)0 and/or (B-V)0 should notbe used for the study of late-type young clusters' members or late-typepre-main sequence stars without some consideration. Instead,near-infrared colours like (R-I)0 should be bettertemperature indicators for these stars.
| 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.
| New periodic variables from the Hipparcos epoch photometry
Two selection statistics are used to extract new candidate periodicvariables from the epoch photometry of the Hipparcos catalogue. Theprimary selection criterion is a signal-to-noise ratio. The dependenceof this statistic on the number of observations is calibrated usingabout 30000 randomly permuted Hipparcos data sets. A significance levelof 0.1 per cent is used to extract a first batch of candidate variables.The second criterion requires that the optimal frequency be unaffectedif the data are de-trended by low-order polynomials. We find 2675 newcandidate periodic variables, of which the majority (2082) are from theHipparcos`unsolved' variables. Potential problems with theinterpretation of the data (e.g. aliasing) are discussed.
| The Catania Automatic Photoelectric Telescope on Mt. Etna: a systematic study of magnetically active stars
A photometric monitoring of about 50 magnetically active stars, that arespread almost all over the H-R diagram, was initiated at the mountainstation of Catania Observatory on Mt. Etna (1750-m a.s.l.) in 1992 withan 80-cm robotic telescope (APT-80) built by AutoScope Co. (USA). Thissystematic survey is now approaching its 10th year anniversary. For mostof the stars, quite well defined solar-like spot maps have been derivedfrom UBV data obtained in different epochs. These data have allowed usto investigate some relevant characteristics of spot activity andvariability on stars, and to obtain clear evidence of long-term activitycycles, in the range from a few to about 10 years, on some of theobserved targets. Starspot maps are constructed by using advanced tools,such as massive parallel computing and are based on Maximum Entropy andTikhonov regularization criteria. Selected results are here presented.Our systematic observation program is still underway and a secondAPT80/2, equipped with a CCD camera, will pair the APT80/1 on the samesite. Its operation is foreseen for mid 2002.
| Long-term monitoring of active stars. IX. Photometry collected in 1993
As a part of an extensive program focused on the global properties andevolution of active stars, high-precision UBV(RI)_c and UBV photometryof 31 selected stars is presented. The UBV(RI)_c observations werecollected at the European Southern Observatory over the 31 December1992-18 January 1993 and the 20 November-3 December 1993 intervals.Additional UBV photometry obtained by the ``Phoenix" and by the CataniaAstrophysical Observatory Automatic Photoelectric Telescopes from 1990to 1993 is also presented for some of the program stars. Significantevolution of the light curves, period variations and evidence forlong-term variability of the global degree of spottedness are found.Some spectral classifications are revised and the inferred photometricparallaxes are compared, whenever possible, with the values measured bythe Hipparcos satellite. These observations are finalized to theconstruction of an extended photometric database, which can giveimportant clues on topics such as the stability of spotted areas,differential rotation, solar-like cycles and the correlation betweeninhomogeneities at different atmospheric levels. Based on data collectedat the European Southern Observatory, La Silla, Chile. Tables and thecomplete data set are also available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/910
| 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
| 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.
| 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 the rotation-activity correlation for active binary stars
We present an investigation of rotation-activity correlations usingInternational Ultraviolet Explorer (IUE) SWP measurements of the Civemission line at 1550Angstroms for 72 active binary systems. We use astandard stellar evolution code to derive non-empirical Rossby numbers,R_0, for each star in our sample and compare the resulting Civrotation-activity correlation to that found for empirically derivedvalues of the Rossby number and that based on rotation alone. For dwarfstars our values of R_0 do not differ greatly from empirical ones and wefind a corresponding lack of improvement in correlation. Only a marginalimprovement in correlation is found for evolved components in oursample. We discuss possible additional factors, other than rotation orconvection, that may influence the activity levels in active binaries.Our observational data imply, in contrast to the theoretical predictionsof convective motions, that activity is only weakly related to mass inevolved stars. We conclude that current dynamo theory is limited in itsapplication to the study of active stars because of the uncertainty inthe angular velocity-depth profile in stellar interiors and the unknowneffects of binarity and surface gravity.
| UBV(RI)_C and UVBY photometry of HD 81410 and starspot distribution in RS CVn objects
We present UBVRI and uvby photometry of HD 81410 obtained on a total of40 nights during 1987-90, and an analysis of its long-term photometricbehaviour. The star is found to show two well-separated minima in itslight curve most of the time; probably there are two preferred effectivelongitudes about which spots are mainly formed. The migration of thephase of the light minimum usually seen in RS CVn stars is absent in HD81410. The rather small spread in the maximum V amplitudes observed inactive RS CVn objects seen at different inclinations of rotational axisimplies that the longitudinal asymmetry in the distribution of spots,which causes the light modulation, is largely restricted to withinaround +/-40(deg) latitudes. The total ranges of rotational periodswhich are quoted in the literature for several spotted stars based onlong-term photometry also imply a similar latitudinal extent of spotsabout the equator. We find that the light and colour curves produced byan equatorial band of spots limited by latitudes and covering the fullrange of longitudes across the hemisphere visible at light minimum canbe approximated reasonably well by two well-separated circular spots.Further, we find that the net effect in the colours produced bylimb-darkening depends on the exact distribution of spots on the stellarsurface; it could be even negligible for certain spot distributions.From the spot modeling of the light and colour curves of HD 81410 wefind that the maximum temperature difference between the photosphere andspots is around 1400 K. We also find that the light modulation is causedby several small individual spots, and during the epochs of shallowminimum spots are spread out, both latitudinally and longitudinally,over a wider region, as indicated by a higher temperature for theequivalent circular spots at those epochs. It seems that in RS CVn starsthe spots occur largely distributed about the equator as in the case ofthe Sun and the solutions which indicate polar spots result fromlimiting the number of spots in the modeling to a few. Based on theobservations collected at the European Southern Observatory, La Silla
| 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)
| The Hyades: distance, structure, dynamics, and age
{We use absolute trigonometric parallaxes from the Hipparcos Catalogueto determine individual distances to members of the Hyades cluster, fromwhich the 3-dimensional structure of the cluster can be derived.Inertially-referenced proper motions are used to rediscuss distancedeterminations based on convergent-point analyses. A combination ofparallaxes and proper motions from Hipparcos, and radial velocities fromground-based observations, are used to determine the position andvelocity components of candidate members with respect to the clustercentre, providing new information on cluster membership: 13 newcandidate members within 20 pc of the cluster centre have beenidentified. Farther from the cluster centre there is a gradual mergingbetween certain cluster members and field stars, both spatially andkinematically. Within the cluster, the kinematical structure is fullyconsistent with parallel space motion of the component stars with aninternal velocity dispersion of about 0.3 km s(-1) . The spatialstructure and mass segregation are consistent with N-body simulationresults, without the need to invoke expansion, contraction, rotation, orother significant perturbations of the cluster. The quality of theindividual distance determinations permits the cluster zero-age mainsequence to be accurately modelled. The helium abundance for the clusteris determined to be Y =3D 0.26+/-0.02 which, combined with isochronemodelling including convective overshooting, yields a cluster age of625+/-50 Myr. The distance to the observed centre of mass (a conceptmeaningful only in the restricted context of the cluster memberscontained in the Hipparcos Catalogue) is 46.34+/-0.27 pc, correspondingto a distance modulus m-M=3D3.33+/-0.01 mag for the objects within 10 pcof the cluster centre (roughly corresponding to the tidal radius). Thisdistance modulus is close to, but significantly better determined than,that derived from recent high-precision radial velocity studies,somewhat larger than that indicated by recent ground-based trigonometricparallax determinations, and smaller than those found from recentstudies of the cluster convergent point. These discrepancies areinvestigated and explained. } Based on observations made with the ESAHipparcos astrometry satellite. Table~2 is also available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http://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)
| Accurate Positions for Radio Stars as Determined from CCD Observations in the Extragalactic Reference Frame.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.1679S&db_key=AST
| Multiwavelength optical observations of chromospherically active binary systems. I. Simultaneous H alpha, NA i D1, D2, and He i D3 observations
This is the first paper of a series aimed at studying the chromosphereof active binary systems using the information provided for severaloptical spectroscopic features. Simultaneous H alpha, Na iD1, D2, and He i D3 spectroscopicobservations are reported here for 18 systems. The chromosphericcontribution in these lines have been determined using the spectralsubtraction technique. Very broad wings have been found in thesubtracted H alpha profile of some of the more active stars. Theseprofiles are well matched using a two-components Gaussian fit (narrowand broad) and the broad component could be interpreted as arising frommicroflaring. Prominence-like extended material have been detected in anear-eclipse H alpha observation of the system AR Lac. The excessemission found in the Na i D1 and D2 lines byapplication of the spectral subtraction technique and the behaviour ofthe H alpha line in the corresponding simultaneous observations indicatethat the filling-in of the core of these lines is a chromosphericactivity indicator. For giant stars of the sample the He i D3line has been detected in absorption in the subtracted spectra. Anoptical flare has been detected in UX Ari and II Peg through thepresence of the He i D3 in emission in coincidence with theenhancement of the H alpha emission. Based on observations made with theIsaac Newton telescope operated on the island of La Palma by the RoyalGreenwich Observatory at the Spanish Observatorio del Roque de LosMuchachos of the Instituto de Astrofisica de Canarias.
| 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.
| 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)
| HD 12545, A Study in Spottedness
We have solved two sets of light curves of HD 12545 at its epoch ofextreme spottedness in 1990-91, one of which coincides with anindependent set analyzed recently by Strassmeier and Olah. Even for thehuge amplitudes observed, these light-curve solutions did not givereliable determinations of several important spot properties.Specifically, we find that we could obtain acceptable solutions for awide range of inclination; that spot temperature depends on inclinationassumed, falling in the range Delta-T = T_star - T_spot = 650-1200 K forinclinations of 70-30 deg; that spot latitudes derived from the lightcurves are unreliable; and that our independent spot solutions disagreewith Strassmeier and Olah's. On a more positive note, changes in thelight curve over the past five years seem to have been caused primarilyby rearrangement of persisting spot groups, and we note that the highlevel of activity implied by its H-alpha emission, makes HD 12545 aprime candidate for a white-light flare star. (SECTION: Stars)
| Random Spots on Chromospherically Active Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996ApJ...462..888E&db_key=AST
| Optical positions of radio stars. I.
The optical positions of 31 radio stars obtained from the observationswith the photoelectric astrolabe at Yunnan Observatory are presented inthis paper. These are all the stars in the astrometric catalogue ofradio stars observable by our astrolabe.
| 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.
| 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.
| Starspot evolution, differential rotation, and magnetic cycles in the chromospherically active binaries lambda andromedae, sigma Geminorum, II Pegasi, and V711 Tauri
We have analyzed 15-19 yr of photoelectric photometry, obtained manuallyand with automated telescopes, of the chromospherically active binarieslambda And, sigma Gem, II Peg, and V711 Tau. These observations let usidentify individual dark starspots on the stellar surfaces from periodicdimming of the starlight, follow the evolution of these spots, andsearch for long-term cyclic changes in the properties of these starspotsthat might reveal magnetic cycles analogous to the Sun's 11 yr sunspotcycle. We developed a computer code to fit a simple two-spot model toour observed light curves that allows us to extract the most easilydeterminable and most reliable spot parameters from the light curves,i.e., spot longitudes and radii. We then used these measured propertiesto identify individual spots and to chart their life histories byconstructing migration and amplitude curves. We identified and followed11 spots in lambda And, 16 in sigma Gem, 12 in II Peg, and 15 in V711Tau. Lifetimes of individual spots ranged from a few months to longerthan 6 yr. Differential rotation coefficients, estimated from theobserved range of spot rotation periods for each star and defined byequation (2), were 0.04 for lambda And, 0.038 for sigma Gem, 0.005 forII Peg, and 0.006 for V711 Tau, versus 0.19 for the Sun. We searched forcyclic changes in mean brightness, B-V color index, and spot rotationperiod as evidence for long-term cycles. Of these, long-term variabilityin mean brightness appears to offer the best evidence for such cycles inthese four stars. Cycles of 11.1 yr for lambda And, 8.5 yr for sigmaGem, 11 yr for II Peg, and 16 yr V711 Tau are implied by these meanbrightness changes. Cyclic changes in spot rotation period were found inlambda And and possibly II Peg. Errors in B-V were too large for anylong-term changes to be detectable.
| 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.
| Excess Hα emission in chromospherically active binaries: the spectroscopic survey.
We present new spectroscopic Hα observations for a sample of 24chromospherically active binary systems (RS CVn and BY Dra classes), ofdifferent activity levels. By using the spectral subtraction technique(subtraction of a synthesized stellar spectrum constructed fromreference stars of similar spectral type and luminosity class) we obtainthe active-chromosphere contribution to the Hα line. The Hαemissions arising from each individual star were obtained when it waspossible to deblend the contribution of both components.
| Lithium, X-ray activity and rotation in an X-ray selected sample of solar-type stars
We present an analysis of the connection between X-ray activity level,photospheric abundance of lithium and surface rotation in late typeactive main sequence stars (G and K), using the ratio between opticaland X-ray luminosity fx/fv as an uniform activity indicator. We performthis analysis for a sample of X-ray selected sources from Einstein-basedsurveys compared to stars from the Pleiades open cluster and to a sampleof active binary stars. We show that these parameters show differentdegrees of statistical correlation in the three samples. In particular,the Pleiades sample shows a significant correlation between all threequantities, while in the X-ray selected sample lithium and rotation aresignificantly correlated with each other but neither is correlated withthe activity level. No correlation is evident for the three quantitiesstudied in the active binary sample. We show how the behavior of theX-ray selected sample can be used to discriminate among differenthypothesis about the nature of the so-called `yellow star excess'observed in X-ray flux-limited surveys, showing that this is composed bya population of young, near Zero-Age Main Sequence (ZAMS) stars withcharacteristics similar to the Pleiades.
| Excess Hα emission in chromospherically active binaries.
We study the behaviour of the excess Hα emission in a sample of 51chromospherically active binary systems (RS CVn and BY Dra classes), ofdifferent activity levels. This sample include the 27 stars analysed byFernandez-Figueroa et al. (1994) and the new observations of 24 systemsdescribed by Montes et al. (1994b). By using the spectral subtractiontechnique (subtraction of a synthesized stellar spectrum constructedfrom reference stars of similar spectral type and luminosity class) weobtain the active-chromosphere contribution to the Hα line inthese 51 systems. We have determined the excess Hα emissionequivalent widths and converted it to surface fluxes. The Hαemissions arising from each component star were obtained when it waspossible to deblend both contributions. The comparison of the excessHα emission, obtained with the spectral subtraction technique,with other Hα activity indices allows us to conclude that this isthe preferable activity indicator for binaries. The behaviour of theexcess Hα emission as a function of the rotation has beenanalyzed. A slight decline toward longer rotational periods, P_rot_, andlarger Rossby numbers, R_0_, is present in agreement with previousresults using others activity indicators. We have compared the derivedexcess Hα emission fluxes with those obtained in the Ca II K andHɛ lines finding that a good correlation exits between thesethree chromospheric activity indicators. The Hα losses seem to bemore important than Ca II K losses for cooler stars, in fact all thesystem with Hα emission above the continuum are cooler than 5000K.Correlations with other activity indicators, (C IV in the transitionregion, and X-rays in the corona) indicate that the exponents of thepower-law relations increase with the formation temperature of thespectral features.
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Pozíciós és asztrometriai adatok
| Csillagkép: | Orion |
| Rektaszcenzió: | 05h41m26.79s |
| Deklináció: | +03°46'40.9" |
| Vizuális fényesség: | 6.828 |
| Távolság: | 144.3 parszek |
| RA sajátmozgás: | 34.1 |
| Dec sajátmozgás: | 5.3 |
| B-T magnitude: | 8.277 |
| V-T magnitude: | 6.948 |
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