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Публикации по объекту
Lithium abundances of the local thin disc stars
Lithium abundances are presented for a sample of 181 nearby F and Gdwarfs with accurate Hipparcos parallaxes. The stars are on circularorbits about the Galactic centre and, hence, are identified as belongingto the thin disc. This sample is combined with two published surveys toprovide a catalogue of lithium abundances, metallicities ([Fe/H]),masses, and ages for 451 F-G dwarfs, almost all belonging to the thindisc. The lithium abundances are compared and contrasted with publishedlithium abundances for F and G stars in local open clusters. The fieldstars span a larger range in [Fe/H] than the clusters for which [Fe/H]~=0.0 +/- 0.2. The initial (i.e. interstellar) lithium abundance of thesolar neighbourhood, as derived from stars for which astration oflithium is believed to be unimportant, is traced from logɛ(Li) =2.2 at [Fe/H]=-1 to logɛ(Li) = 3.2 at +0.1. This form for theevolution is dependent on the assumption that astration of lithium isnegligible for the stars defining the relation. An argument is advancedthat this latter assumption may not be entirely correct, and, theevolution of lithium with [Fe/H] may be flatter than previouslysupposed. A sharp Hyades-like Li dip is not seen among the field starsand appears to be replaced by a large spread among lithium abundances ofstars more massive than the lower mass limit of the dip. Astration oflithium by stars of masses too low to participate in the Li dip isdiscussed. These stars show little to no spread in lithium abundance ata given [Fe/H] and mass.
| Chemical enrichment and star formation in the Milky Way disk. III. Chemodynamical constraints
In this paper, we investigate some chemokinematical properties of theMilky Way disk, by using a sample composed by 424 late-type dwarfs. Weshow that the velocity dispersion of a stellar group correlates with theage of this group, according to a law proportional to t0.26,where t is the age of the stellar group. The temporal evolution of thevertex deviation is considered in detail. It is shown that the vertexdeviation does not seem to depend strongly on the age of the stellargroup. Previous studies in the literature seem to not have found it dueto the use of statistical ages for stellar groups, rather thanindividual ages. The possibility to use the orbital parameters of a starto derive information about its birthplace is investigated, and we showthat the mean galactocentric radius is likely to be the most reliablestellar birthplace indicator. However, this information cannot bepresently used to derive radial evolutionary constraints, due to anintrinsic bias present in all samples constructed from nearby stars. Anextensive discussion of the secular and stochastic heating mechanismscommonly invoked to explain the age-velocity dispersion relation ispresented. We suggest that the age-velocity dispersion relation couldreflect the gradual decrease in the turbulent velocity dispersion fromwhich disk stars form, a suggestion originally made by Tinsley &Larson (\cite{tinsley}, ApJ, 221, 554) and supported by several morerecent disk evolution calculations. A test to distinguish between thetwo types of models using high-redshift galaxies is proposed.Full Table 1 is only 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/423/517
| The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of 14 000 F and G dwarfs
We present and discuss new determinations of metallicity, rotation, age,kinematics, and Galactic orbits for a complete, magnitude-limited, andkinematically unbiased sample of 16 682 nearby F and G dwarf stars. Our63 000 new, accurate radial-velocity observations for nearly 13 500stars allow identification of most of the binary stars in the sampleand, together with published uvbyβ photometry, Hipparcosparallaxes, Tycho-2 proper motions, and a few earlier radial velocities,complete the kinematic information for 14 139 stars. These high-qualityvelocity data are supplemented by effective temperatures andmetallicities newly derived from recent and/or revised calibrations. Theremaining stars either lack Hipparcos data or have fast rotation. Amajor effort has been devoted to the determination of new isochrone agesfor all stars for which this is possible. Particular attention has beengiven to a realistic treatment of statistical biases and errorestimates, as standard techniques tend to underestimate these effectsand introduce spurious features in the age distributions. Our ages agreewell with those by Edvardsson et al. (\cite{edv93}), despite severalastrophysical and computational improvements since then. We demonstrate,however, how strong observational and theoretical biases cause thedistribution of the observed ages to be very different from that of thetrue age distribution of the sample. Among the many basic relations ofthe Galactic disk that can be reinvestigated from the data presentedhere, we revisit the metallicity distribution of the G dwarfs and theage-metallicity, age-velocity, and metallicity-velocity relations of theSolar neighbourhood. Our first results confirm the lack of metal-poor Gdwarfs relative to closed-box model predictions (the ``G dwarfproblem''), the existence of radial metallicity gradients in the disk,the small change in mean metallicity of the thin disk since itsformation and the substantial scatter in metallicity at all ages, andthe continuing kinematic heating of the thin disk with an efficiencyconsistent with that expected for a combination of spiral arms and giantmolecular clouds. Distinct features in the distribution of the Vcomponent of the space motion are extended in age and metallicity,corresponding to the effects of stochastic spiral waves rather thanclassical moving groups, and may complicate the identification ofthick-disk stars from kinematic criteria. More advanced analyses of thisrich material will require careful simulations of the selection criteriafor the sample and the distribution of observational errors.Based on observations made with the Danish 1.5-m telescope at ESO, LaSilla, Chile, and with the Swiss 1-m telescope at Observatoire deHaute-Provence, France.Complete Tables 1 and 2 are only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/989
| On the link between rotation, chromospheric activity and Li abundance in subgiant stars
The connection rotation-CaII emission flux-lithium abundance is analyzedfor a sample of bona fide subgiant stars, with evolutionary statusdetermined from HIPPARCOS trigonometric parallax measurements and fromthe Toulouse-Geneva code. The distribution of rotation and CaII emissionflux as a function of effective temperature shows a discontinuitylocated around the same spectral type, F8IV. Blueward of this spectraltype, subgiants have a large spread of values of rotation and CaII flux,whereas stars redward of F8IV show essentially low rotation and low CaIIflux. The strength of these declines depends on stellar mass. Theabundance of lithium also shows a sudden decrease. For subgiants withmass lower than about 1.2 Msun the decrease is located laterthan that in rotation and CaII flux, whereas for masses higher than 1.2Msun the decrease in lithium abundance is located around thespectral type F8IV. The discrepancy between the location of thediscontinuities of rotation and CaII emission flux and log n(Li) forstars with masses lower than 1.2 Msun seems to reflect thesensitivity of these phenomena to the mass of the convective envelope.The drop in rotation, which results mostly from a magnetic braking,requires an increase in the mass of the convective envelope less thanthat required for the decrease in log n(Li). The location of thediscontinuity in log n(Li) for stars with masses higher than 1.2Msun, in the same region of the discontinuities in rotationand CaII emission flux, may also be explained by the behavior of thedeepening of the convective envelope. The more massive the star is, theearlier is the increase of the convective envelope. In contrast to therelationship between rotation and CaII flux, which is fairly linear, therelationship between lithium abundance and rotation shows no cleartendency toward linear behavior. Similarly, no clear linear trend isobserved in the relationship between lithium abundance and CaII flux. Inspite of these facts, subgiants with high lithium content also have highrotation and high CaII emission flux.
| Statistical cataloging of archival data for luminosity class IV-V stars. II. The epoch 2001 [Fe/H] catalog
This paper describes the derivation of an updated statistical catalog ofmetallicities. The stars for which those metallicities apply are ofspectral types F, G, and K, and are on or near the main sequence. Theinput data for the catalog are values of [Fe/H] published before 2002February and derived from lines of weak and moderate strength. Theanalyses used to derive the data have been based on one-dimensional LTEmodel atmospheres. Initial adjustments which are applied to the datainclude corrections to a uniform temperature scale which is given in acompanion paper (see Taylor \cite{t02}). After correction, the data aresubjected to a statistical analysis. For each of 941 stars considered,the results of that analysis include a mean value of [Fe/H], an rmserror, an associated number of degrees of freedom, and one or moreidentification numbers for source papers. The catalog of these resultssupersedes an earlier version given by Taylor (\cite{t94b}).Catalog is only available in electronic form at the CDS via anonymousftp cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/398/731
| Statistical cataloging of archival data for luminosity class IV-V stars. I. The epoch 2001 temperature catalog
This paper is one of a pair in which temperatures and metallicitycatalogs for class IV-V stars are considered. The temperature catalogdescribed here is derived from a calibration based on stellar angulardiameters. If published calibrations of this kind are compared by usingcolor-index transformations, temperature-dependent differences among thecalibrations are commonly found. However, such differences are minimizedif attention is restricted to calibrations based on Johnson V-K. Acalibration of this sort from Di Benedetto (\cite{dib98}) is thereforetested and adopted. That calibration is then applied to spectroscopicand photometric data, with the latter predominating. Cousins R-Iphotometry receives special attention because of its high precision andlow metallicity sensitivity. Testing of temperatures derived from thecalibration suggests that their accuracy and precision are satisfactory,though further testing will be warranted as new results appear. Thesetemperatures appear in the catalog as values of theta equiv5040/T(effective). Most of these entries are accompanied by measured orderived values of Cousins R-I. Entries are given for 951 stars.Catalog 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/398/721
| HIPPARCOS age-metallicity relation of the solar neighbourhood disc stars
We derive age-metallicity relations (AMRs) and orbital parameters forthe 1658 solar neighbourhood stars to which accurate distances aremeasured by the HIPPARCOS satellite. The sample stars comprise 1382 thindisc stars, 229 thick disc stars, and 47 halo stars according to theirorbital parameters. We find a considerable scatter for thin disc AMRalong the one-zone Galactic chemical evolution (GCE) model. Orbits andmetallicities of thin disc stars show now clear relation each other. Thescatter along the AMR exists even if the stars with the same orbits areselected. We examine simple extension of one-zone GCE models whichaccount for inhomogeneity in the effective yield and inhomogeneous starformation rate in the Galaxy. Both extensions of the one-zone GCE modelcannot account for the scatter in age - [Fe/H] - [Ca/Fe] relationsimultaneously. We conclude, therefore, that the scatter along the thindisc AMR is an essential feature in the formation and evolution of theGalaxy. The AMR for thick disc stars shows that the star formationterminated 8 Gyr ago in the thick disc. As already reported by Grattonet al. (\cite{Gratton_et.al.2000}) and Prochaska et al.(\cite{Prochaska_et.al.2000}), thick disc stars are more Ca-rich thanthin disc stars with the same [Fe/H]. We find that thick disc stars showa vertical abundance gradient. These three facts, the AMR, verticalgradient, and [Ca/Fe]-[Fe/H] relation, support monolithic collapseand/or accretion of satellite dwarf galaxies as likely thick discformation scenarios. Tables 2 and 3 are only 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/ cgi-bin/qcat?J/ A+A/394/927
| Levels of coronal and chromospheric activity in late-type stars and various types of dynamo waves
We analyze the X-ray emission and chromospheric activity of late-type F,G, and K stars studied in the framework of the HK project. More powerfulcoronas are possessed by stars displaying irregular variations of theirchromospheric emission, while stars with cyclic activity arecharacterized by comparatively modest X-ray luminosities and ratios ofthe X-ray to bolometric luminosity L X/L bol. This indicates that thenature of processes associated with magnetic-field amplification in theconvective envelope changes appreciably in the transition from small tolarge dynamo numbers, directly affecting the character of the(α-Ω) dynamo. Due to the strong dependence of both thedynamo number and the Rossby number on the speed of axial rotation,earlier correlations found between various activity parameters and theRossby number are consistent with our conclusions. Our analysis makes itpossible to draw the first firm conclusions about the place of solaractivity among analogous processes developing in active late-type stars.
| Lithium and rotation on the subgiant branch. II. Theoretical analysis of observations
Lithium abundances and rotation, determined for 120 subgiant stars inLèbre et al. (1999) are analyzed. To this purpose, theevolutionary status of the sample as well as the individual masses havebeen determined using the HIPPARCOS trigonometric parallax measurementsto locate very precisely our sample stars in the HR diagram. We look atthe distributions of A_Li and Vsini with mass when stars evolve from themain sequence to the subgiant branch. For most of the stars in oursample we find good agreement with the dilution predictions. However,the more massive cool stars with upper limits of Li abundances show asignificant discrepancy with the theoretical predictions, even if theNon-LTE effects are taken into account. For the rotation behaviour, ouranalysis confirms that low mass stars leave the main sequence with a lowrotational rate, while more massive stars are slowed down only whenreaching the subgiant branch. We also checked the connection between theobserved rotation behaviour and the magnetic braking due to thedeepening of the convective envelope. Our results shed new light on thelithium and rotation discontinuities in the evolved phase.
| A Second Catalog of Orbiting Astronomical Observatory 2 Filter Photometry: Ultraviolet Photometry of 614 Stars
Ultraviolet photometry from the Wisconsin Experiment Package on theOrbiting Astronomical Observatory 2 (OAO 2) is presented for 614 stars.Previously unpublished magnitudes from 12 filter bandpasses withwavelengths ranging from 1330 to 4250 Å have been placed on thewhite dwarf model atmosphere absolute flux scale. The fluxes wereconverted to magnitudes using V=0 for F(V)=3.46x10^-9 ergs cm^-2 s^-1Å^-1, or m_lambda=-2.5logF_lambda-21.15. This second catalogeffectively doubles the amount of OAO 2 photometry available in theliterature and includes many objects too bright to be observed withmodern space observatories.
| 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
| Lithium in population I subgiants
We present a lithium survey for a sample of 91 Pop. I stars. JHKLphotometry was also obtained for 61 stars in the sample. Besides Liabundances, [Fe/H] values were derived. Thanks to Hipparcos parallaxes,we could infer absolute V magnitudes for our sample stars and were ableto place them on the color-magnitude diagram, which allowed us toconstrain their evolutionary status. Masses and ages were derived formost of the stars by comparison with evolutionary tracks. The sample wasoriginally selected so to include class IV stars later thanspectral-type F0, but, based on the location on the color-magnitudediagram, we found a posteriori that a fraction of the stars (about 20%)are either main sequence stars or evolved giants. As it is the case fordwarfs and giants, a large spread in lithium abundance is present amongthe subgiants in our sample. As expected, the average lithium decreasesas the stars evolve along the subgiant branch; however, there is not aone-to-one relationship between the position on the color-magnitudediagram and lithium abundance, and the observed dispersion is onlypartially explainable as due to a dispersion in mass, metallicity, andage. In particular, a dispersion in lithium is seen among slightlyevolved subgiants with masses close to solar but in the sameevolutionary stage as the G2 IV star beta Hyi. The comparison of thebeta Hyi-like sample with a sample of non evolved solar-like starsindeed suggests that beta Hyi has most likely evolved from a mainsequence Li-rich star, rather than from a Li-poor star (like the Sun)that has dredged-up previously stored lithium. Our sample includesseveral stars that have completed the first-dredge up lithium dilution,but that have not yet evolved to the evolutionary point whereextra-mixing in the giant phase is thought to occur. A large number ofthem have Li abundances considerably below the theoretical predictionsof first dredge-up dilution. We confirm that this is due to the factthat the progenitors of these stars are most likely stars that havedepleted lithium while on the main sequence; the fraction of post-dredgeup Li rich/poor stars, in fact, is consistent with the observeddistribution of Li abundances among stars that have just left the mainsequence. The signature of the second mixing (or RGB extra-mixing)episode is evident in the log n(Li) vs. B-V and log n(Li) vs. M_boldistributions of the stars in the sample; it seems however that theextra-mixing occurs at luminosities lower than predicted by the modelsof Charbonnel (1994). Finally, a few evolved giants are found thatshould have passed the second mixing episode, but that do not show signsof it. At least half of them are spectroscopic binaries. Based onobservations carried out at the European Southern Observatory, La Silla,Chile
| Lithium and rotation on the subgiant branch. I. Observations and spectral analysis
We have obtained new high resolution spectroscopic observations of thelithium line at 6707.81 Angstroms and derived lithium abundances (A_Li )by spectral synthesis for a sample of about 120 F-, G- and K-typePopulation I subgiant stars. For each of these stars, high precisionrotational velocity obtained with the CORAVEL spectrometer is available.We present the behavior of the lithium abundance as a function ofeffective temperature, which shows a sort of discontinuity around 5600K, somewhat later than the well known rotational discontinuity. based onobservations collected at the Observatoire de Haute--Provence (France)and at the European Southern Observatory, La Silla (Chile).
| Chromospheric CaII H and K emission among subdwarfs
Echelle spectra have been obtained of the CaII H and K lines for asample of metal-poor subdwarf stars as well as for a number of nearbyPopulation I dwarfs selected from among those included in the MountWilson HK survey. The main conclusion of this paper is that CaII H- andK-line emission does occur among subdwarfs. It is particularly notableamong those subdwarfs with colours of B-V>=0.75 all such starsobserved exhibit chromospheric emission, although emission is observedamong some subdwarfs bluer than this colour. The CaII K emission profilein most subdwarfs exhibits an asymmetry of V/R>1, similar to thatseen in the integrated light of the solar disc. Two quantitativeindicators of the contrast between the peaks in the emission profile andthe neighbouring photospheric line profile are introduced. Measurementsof these indicators show that the level of CaII emission among thesubdwarfs is similar to that among low-activity Population I dwarfs.
| Patterns of Variation among Sun-like Stars
We examine the patterns of variation among a sample of 35 stars thatincludes the Sun, particularly on the timescale of the 11 yr solaractivity cycle. Our investigation uses contemporaneous photometric andchromospheric HK emission time series measurements from the Lowell andMount Wilson Observatories, and comparable solar data. We find that thephotometric and HK variability of the stars in our sample can be relatedto their average level of chromospheric activity by power laws. Thephotometric variability of the Sun may be somewhat subdued for itsaverage activity level. We find that the younger, more active stars inour sample tend to become fainter as their HK emission increases,whereas the older, less active stars tend to become brighter as their HKemission increases, as the Sun does during its activity cycle.
| Far-Ultraviolet Continuum of G-Type Stars: A Signature of the Temperature Minimum Region
The main results of a program of systematic comparison between observedand computed UV spectral energy distributions of field G-type stars areillustrated. We constructed the UV observed energy distributions for 53G stars, starting from the IUE Uniform Low Dispersion Archive (ULDA) andcomputed the corresponding theoretical fluxes by using the atmosphericparameters from the Catalogue of [Fe/H] Determinations (1996 edition)and a Kurucz grid of model fluxes. From the comparison betweenobservations and classical models, a UV excess shortward of 2000 Åis evident for all the program stars. The UV continuum in the region1600-2000 Å can be described by synthetic fluxes computed fromsemiempirical models based on the temperature minimum concept. Valuesfor the T_min/T_eff ratio on the order of 0.80 are suitable for theinterpretation of the observed fluxes. The residual discrepanciesshortward of 1600 Å are suggested to be effects of thechromosphere, on the basis of a comparison with the Maltby et al.semiempirical model of the Sun.
| Classification of Population II Stars in the Vilnius Photometric System. II. Results
The results of photometric classification of 848 true and suspectedPopulation II stars, some of which were found to belong to Population I,are presented. The stars were classified using a new calibrationdescribed in Paper I (Bartkevicius & Lazauskaite 1996). We combinethese results with our results from Paper I and discuss in greaterdetail the following groups of stars: UU Herculis-type stars and otherhigh-galactic-latitude supergiants, field red horizontal-branch stars,metal-deficient visual binaries, metal-deficient subgiants, stars fromthe Catalogue of Metal-deficient F--M Stars Classified Photometrically(MDPH; Bartkevicius 1993) and stars from one of the HIPPARCOS programs(Bartkevicius 1994a). It is confirmed that high galactic latitudesupergiants from the Bartaya (1979) catalog are giants or even dwarfs.Some stars, identified by Rose (1985) and Tautvaisiene (1996a) as fieldRHB stars, appear to be ordinary giants according to our classification.Some of the visual binaries studied can be considered as physical pairs.Quite a large fraction of stars from the MDPH catalog are found to havesolar metallicity. A number of new possible UU Herculis-type stars, RHBstars and metal-deficient subgiants are identified.
| The Photometric Variability of Sun-like Stars: Observations and Results, 1984--1995
Using differential Stromgren b, y photometry, we monitored thebrightness variations of 41 program stars and their 73 comparison starsfrom 1984 through 1995. The predominantly main-sequence program starsspanned ranges of temperature and mean chromospheric activity centeredon solar values. About 40% of all the stars showed measurablevariability, typically at levels below 0.01 mag (~1%), on bothnight-to-night and year-to-year timescales. The variability correlatedwith mean chromospheric activity and advancing spectral type. We presentdifferential light curves and statistical descriptions of ourobservations.
| A catalogue of [Fe/H] determinations: 1996 edition
A fifth Edition of the Catalogue of [Fe/H] determinations is presentedherewith. It contains 5946 determinations for 3247 stars, including 751stars in 84 associations, clusters or galaxies. The literature iscomplete up to December 1995. The 700 bibliographical referencescorrespond to [Fe/H] determinations obtained from high resolutionspectroscopic observations and detailed analyses, most of them carriedout with the help of model-atmospheres. The Catalogue is made up ofthree formatted files: File 1: field stars, File 2: stars in galacticassociations and clusters, and stars in SMC, LMC, M33, File 3: numberedlist of bibliographical references The three files are only available inelectronic form at the Centre de Donnees Stellaires in Strasbourg, viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Library of high and mid-resolution spectra in the CA II H & K, Hα, Hβ NA i D1, D2, and He i D3 line regions of F, G, K and M field stars
In this work we present spectroscopic observations centered in thespectral lines most widely used as optical indicators of chromosphericactivity (Hα, Hβ, Ca ii H & K, and He i D3) ina sample of F, G, K and M chromospherically inactive stars. The spectrahave been obtained with the aim of providing a library of high andmid-resolution spectra to be used in the application of the spectralsubtraction technique to obtain the active-chromosphere contribution tothese lines in chromospherically active single and binary stars. Thislibrary can also be used for spectral classification purposes. A digitalversion with all the spectra is available via ftp and the World Wide Web(WWW) in both ASCII and FITS formats. Based on observations made withthe Isaac Newton telescope and the William Herschel Telescope operatedon the island of La Palma by the Royal Greenwich Observatory at theSpanish Observatorio del Roque de Los Muchachos of the Instituto deAstrofisica de Canarias, and with the 2.2 m telescope of the CentroAstronomico Hispano-Aleman of Calar Alto (Almeria, Spain) operatedjointly by the Max Planck Institut fur Astronomie (Heidelberg) and theSpanish Comision Nacional de Astronomia. The spectra of the stars listedin Table \protect\ref{tab:par} are also available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| On the link between rotation and lithium depletion in subgiant stars.
We present projected rotational velocity Vsini for 65 F, G and Ksubgiant stars. In this work we study the link between rotation andLithium abundance in such class of luminosity. In particular, we lookfor possible effects of rotational braking on the Lithium depletion. Weshow that a sharp decrease in Lithium abundances parallels therotational discontinuity, located at F8IV, in all its aspects. We havefound some dependence of Lithium abundance upon rotation for singlesubgiants, but there is no evident correlation between Lithium abundanceand rotational velocity for binary subgiant stars.
| Magnetic Field and Rotation in Lower Main-Sequence Stars: an Empirical Time-dependent Magnetic Bode's Relation?
We find a significant correlation between the magnetic and rotationalmoments for a sample of 112 lower main-sequence stars. The rotationalmoment is calculated from measurements of the rotation period in most ofthe stars (not from the projected rotational velocity inferred fromDoppler broadening). The magnetic moment is computed from a database ofhomogeneous measurements of the mean level of Ca II H and K emissionfluxes sampled for most of the stars over an interval of 25 yr. Theslope connecting the logarithm of the magnetic moment and the logarithmof the rotational moment is about +0.5--0.6, with a Pearson correlationcoefficient of about +0.9. The scatter of points from the mean relationhas a component that is natural and caused by decade-long surfacevariability.
| Photometric survey near the main Galactic meridian: 2.1. Finding charts and photoelectric U,B,V,R stellar magnitudes in 25 fields
Finding charts and photoelectric U,B,V,R magnitudes of stars in 25fields in the Main Galactic Meridian (programme MEGA) are presented.This part of the photometric survey includes fields near the NorthGalactic pole and fields at southern Galactic latitudes. Together withthe finding charts of 2.5(deg) x2.5(deg) the equatorial coordinates ofthe stars are given for epoch and equinox 1950.
| The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC).
The positions of 53 FK5, 70 FK5 Extension and 486 GC stars are given forthe equator and equinox J2000.0 and for the mean observation epoch ofeach star. They are determined with the photoelectric astrolabe ofYunnan Observatory. The internal mean errors in right ascension anddeclination are +/- 0.046" and +/- 0.059", respectively. The meanobservation epoch is 1989.51.
| Coronal X-ray emission of cool stars in relation to chromospheric activity and magnetic cycles.
We study the relationship between the coronal X-ray emission of single,main-sequence F-K stars and the characteristics of their magneticcycles. We use X-ray data primarily from the ROSAT all-sky survey (RASS)as well as data acquired by us in the ROSAT pointed program, and thepublished data of the Mt. Wilson CaII H+K monitoring program. Accordingto their CaII H+K long-term variability characteristics, we divide thestars into three groups: non-variable, regular variable and irregular(chaotic) variable stars. We show that the regular and the irregularstars differ mainly in their Rossby-numbers (Ro): regular stars havealmost always Ro<1 whereas the irregular group is characterized byRo>1 further, the X-ray surface flux distributions differsignificantly between these three groups. We discuss to what extentstars exhibiting constant Ca II fluxes can be considered "Maunderminimum" stars, and demonstrate - in a statistical sense - that cyclicchromospheric activity also implies cyclic coronal activity. From areanalysis of the flux-flux relation between the calcium excess fluxdensity ({DELTA}F_Ca_) and F_X_, we find different relations between theregular and the constant stars on one hand and the irregular stars onthe other hand. Performing regression analysis in the form of a powerlaw, the coefficient κ is derived to be κ=~1 for constantand regular stars whereas κ=~2 for the more active irregularstars. We discuss our findings in the context of a transition from anonlinear to a linear dynamo regime when going from irregular to regularstars.
| The solar-stellar spectrograph: Project description, data calibration, and initial results
The Solar-Stellar Spectrograph (SSS) is a project initiated in the 1980sby scientists from the High Altitude Observatory, Lowell Observatory,the Pennsylvania State Universty, and the Sacramento Peak Observatory.The instrument is comprised of two spectrographs: one is an echellecovering the wavelength range lambda lambda 5000-9200, while the secondis a Littrow spectrograph covering the Ca II and H and K region aroundlambda 3950. This project is designed to address a broad range ofoutstanding questions regarding the nature of stellar activity cycles.The unique capability of the spectrograph is its ability to record bothsolar and stellar spectra, allowing more accurate placement of the Sunin the stellar context than has been feasible previously. In this reportwe discuss the motivation for this project, the instrumentalcharacteristics, the observing programs, the methods being used toreduce, calibrate, and analyze the data, and the connection of ourdatabases to extant databases. A central part of the discussion is theconnection of the Sun with the stars both in terms of existing solar andstellar activity indices as well as physical flux. This work resolves along-standing discrepancy in this area and establishes a protocol forrelating the large set of observations from the Mount Wilson Ca II H andK project to physical flux, in preparation for future comparison to ourobservations and results from theory.
| Chromospheric variations in main-sequence stars
The fluxes in passbands 0.1 nm wide and centered on the Ca II H and Kemission cores have been monitored in 111 stars of spectral type F2-M2on or near the main sequence in a continuation of an observing programstarted by O. C. Wilson. Most of the measurements began in 1966, withobservations scheduled monthly until 1980, when observations werescheduled sevral times per week. The records, with a long-term precisionof about 1.5%, display fluctuations that can be identified withvariations on timescales similar to the 11 yr cycle of solar activity aswell as axial rotation, and the growth and decay of emitting regions. Wepresent the records of chromospheric emission and general conclusionsabout variations in surface magnetic activity on timescales greater than1 yr but less than a few decades. The results for stars of spectral typeG0-K5 V indicate a pattern of change in rotation and chromosphericactivity on an evolutionary timescale, in which (1) young stars exhibithigh average levels of activity, rapid rotation rates, no Maunderminimum phase and rarely display a smooth, cyclic variation; (2) starsof intermediate age (approximately 1-2 Gyr for 1 solar mass) havemoderate levels of activity and rotation rates, and occasional smoothcycles; and (3) stars as old as the Sun and older have slower rotationrates, lower activity levels and smooth cycles with occasional Maunderminimum-phases.
| Photometric Survey Near the Main Galactic Meridian - Part One - Photoelectric Stellar Magnitudes and Colours in the UBVR System
Not Available
| Ca II H and K Filter Photometry on the UVBY System. II. The Catalog of Observations
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....109.2828T&db_key=AST
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
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Группы:
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Наблюдательные данные и астрометрия
| Созвездие: | Кит |
| Прямое восхождение: | 02h11m21.10s |
| Склонение: | +08°34'11.0" |
| Видимая звёздная величина: | 5.63 |
| Расстояние: | 42.517 парсек |
| Собственное движение RA: | -141.9 |
| Собственное движение Dec: | -114.1 |
| B-T magnitude: | 6.309 |
| V-T magnitude: | 5.689 |
Каталоги и обозначения:
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