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New insights on the AU-scale circumstellar structure of FU Orionis
We report new near-infrared, long-baseline interferometric observationsat the AU scale of the pre-main-sequence star FU Orionis with the PTI,IOTA and VLTI interferometers. This young stellar object has beenobserved on 42 nights over a period of 6 years from 1998 to 2003. Wehave obtained 287 independent measurements of the fringe visibility with6 different baselines ranging from 20 to 110 m in length, in the H and Kbands. Our data resolves FU Ori at the AU scale, and provides newconstraints at shorter baselines and shorter wavelengths. Our extensive(u,v)-plane coverage, coupled with the published spectral energydistribution data, allows us to test the accretion disk scenario. Wefind that the most probable explanation for these observations is thatFU Ori hosts an active accretion disk whose temperature law isconsistent with standard models and with an accretion rate of dot M=(6.3 ± 0.6) × 10-5(Mstar/Mȯ)-1 Mȯyr-1. We are able to constrain the geometry of the disk,including an inclination of 55-7+5 deg and aposition angle of 47-11 0+7 deg. In addition, a 10percent peak-to-peak oscillation is detected in the data (at thetwo-sigma level) from the longest baselines, which we interpret as apossible disk hot-spot or companion. The still somewhat limited (u, v)sampling and substantial measurement uncertainty prevent us fromconstraining the location of the spot with confidence, since manysolutions yield a statistically acceptable fit. However, the oscillationin our best data set is best explained with an unresolved spot locatedat a projected distance of 10 ± 1 AU at the 130 ± 1 degposition angle and with a magnitude difference of Δ K ≈ 3.9± 0.2 and Δ H ≈ 3.6 ± 0.2 mag moving away fromthe center at a rate of 1.2 ± 0.6 AU yr-1. Althoughthis bright spot on the surface of the disk could be tracing somethermal instabilities in the disk, we propose to interpret this spot asthe signature of a companion of the central FU Ori system on anextremely eccentric orbit. We speculate that the close encounter of thisputative companion and the central star could be the explanation of theinitial photometric rise of the luminosity of this object.
| CHARM2: An updated Catalog of High Angular Resolution Measurements
We present an update of the Catalog of High Angular ResolutionMeasurements (CHARM, Richichi & Percheron \cite{CHARM}, A&A,386, 492), which includes results available until July 2004. CHARM2 is acompilation of direct measurements by high angular resolution methods,as well as indirect estimates of stellar diameters. Its main goal is toprovide a reference list of sources which can be used for calibrationand verification observations with long-baseline optical and near-IRinterferometers. Single and binary stars are included, as are complexobjects from circumstellar shells to extragalactic sources. The presentupdate provides an increase of almost a factor of two over the previousedition. Additionally, it includes several corrections and improvements,as well as a cross-check with the valuable public release observationsof the ESO Very Large Telescope Interferometer (VLTI). A total of 8231entries for 3238 unique sources are now present in CHARM2. Thisrepresents an increase of a factor of 3.4 and 2.0, respectively, overthe contents of the previous version of CHARM.The catalog is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/431/773
| ARIES imaging polarimeter.
An Imaging Polarimeter has been fabricated for use with liquid- N2cooled CCD camera and is designed to suit 104-cm Sampurnanand telescopewith an f/13 focus at Aryabhatta Research Institute of ObservationalSciences (ARIES), Naini Tal. The instrument measures the linearpolarisation in broad B, V and R band and has a field of view ~ 20' x20'. We are presenting here some observations regarding the polarisationof some polarised as well as unpolarised stars with a view to show theperformance of our polarimeter.
| Nearby stars of the Galactic disk and halo. III.
High-resolution spectroscopic observations of about 150 nearby stars orstar systems are presented and discussed. The study of these and another100 objects of the previous papers of this series implies that theGalaxy became reality 13 or 14 Gyr ago with the implementation of amassive, rotationally-supported population of thick-disk stars. The veryhigh star formation rate in that phase gave rise to a rapid metalenrichment and an expulsion of gas in supernovae-driven Galactic winds,but was followed by a star formation gap for no less than three billionyears at the Sun's galactocentric distance. In a second phase, then, thethin disk - our ``familiar Milky Way'' - came on stage. Nowadays ittraces the bright side of the Galaxy, but it is also embedded in a hugecoffin of dead thick-disk stars that account for a large amount ofbaryonic dark matter. As opposed to this, cold-dark-matter-dominatedcosmologies that suggest a more gradual hierarchical buildup throughmergers of minor structures, though popular, are a poor description forthe Milky Way Galaxy - and by inference many other spirals as well - if,as the sample implies, the fossil records of its long-lived stars do notstick to this paradigm. Apart from this general picture that emergeswith reference to the entire sample stars, a good deal of the presentwork is however also concerned with detailed discussions of manyindividual objects. Among the most interesting we mention the bluestraggler or merger candidates HD 165401 and HD 137763/HD 137778, thelikely accretion of a giant planet or brown dwarf on 59 Vir in itsrecent history, and HD 63433 that proves to be a young solar analog at\tau200 Myr. Likewise, the secondary to HR 4867, formerly suspectednon-single from the Hipparcos astrometry, is directly detectable in thehigh-resolution spectroscopic tracings, whereas the visual binary \chiCet is instead at least triple, and presumably even quadruple. Withrespect to the nearby young stars a complete account of the Ursa MajorAssociation is presented, and we provide as well plain evidence foranother, the ``Hercules-Lyra Association'', the likely existence ofwhich was only realized in recent years. On account of its rotation,chemistry, and age we do confirm that the Sun is very typical among itsG-type neighbors; as to its kinematics, it appears however not unlikelythat the Sun's known low peculiar space velocity could indeed be thecause for the weak paleontological record of mass extinctions and majorimpact events on our parent planet during the most recent Galactic planepassage of the solar system. Although the significance of thiscorrelation certainly remains a matter of debate for years to come, wepoint in this context to the principal importance of the thick disk fora complete census with respect to the local surface and volumedensities. Other important effects that can be ascribed to this darkstellar population comprise (i) the observed plateau in the shape of theluminosity function of the local FGK stars, (ii) a small thoughsystematic effect on the basic solar motion, (iii) a reassessment of theterm ``asymmetrical drift velocity'' for the remainder (i.e. the thindisk) of the stellar objects, (iv) its ability to account for the bulkof the recently discovered high-velocity blue white dwarfs, (v) itsmajor contribution to the Sun's 220 km s-1 rotationalvelocity around the Galactic center, and (vi) the significant flatteningthat it imposes on the Milky Way's rotation curve. Finally we note ahigh multiplicity fraction in the small but volume-complete local sampleof stars of this ancient population. This in turn is highly suggestivefor a star formation scenario wherein the few existing single stellarobjects might only arise from either late mergers or the dynamicalejection of former triple or higher level star systems.
| A new Böhm-Vitense gap in the temperature range 5560 to 5610 K in the main sequence hm-Vitense gap in the main sequence
Highly precise temperatures (σ = 10-15 K) have been determinedfrom line depth ratios for a set of 248 F-K field dwarfs of about solarmetallicity (-0.5 < [Fe/H] < +0.4), based on high resolution (R=42000), high S/N echelle spectra. A new gap has been discovered in thedistribution of stars on the Main Sequence in the temperature range 5560to 5610 K. This gap coincides with a jump in the microturbulent velocityVt and the well-known Li depression near 5600 K in fielddwarfs and open clusters. As the principal cause of the observeddiscontinuities in stellar properties we propose the penetration of theconvective zone into the inner layers of stars slightly less massivethan the Sun and related to it, a change in the temperature gradient.Based on spectra collected with the ELODIE spectrograph at the 1.93-mtelescope of the Observatoire de Haute-Provence (France).Full Table 1 is only available in electronic form athttp://www.edpsciences.org
| 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
| Polarimetric evolution of V838 Monocerotis
We present the results of our polarimetric and spectropolarimetricmonitoring of V838 Monocerotis, performed at the Asiago and Crimeanobservatories during and after the multiple outbursts that occurred inJanuary-March 2002. The polarization of the object is mainly due tointerstellar polarization (P 2.48%). Intrinsic polarization up to 0.7% at 5000 Å is present during the second maximum of theobject (February 2002). This intrinsic component increases towardshorter wavelengths but our limited spectral coverage (5000-7500Å) does not allow conclusive inferences about its origin. A strongdepolarization across the Hα profile is observed. Theinterstellar polarization gives a lower limit to the reddening of E(B-V)>0.28, with E(B-V) 0.5 being the most probable value. A normalratio of total to selective absorption (RV=3.22±0.17)was derived from the wavelength of maximum interstellar polarization.This suggests a low (if any) contribution by circumstellar material witha peculiar dust to gas ratio. A polarimetric map of a portion of thelight echo shows a complex polarization distribution reachingPmax=45%.Based on observations collected at Padua Astronomical Observatory atAsiago and Crimean Astrophysical Observatory.
| Some anomalies in the occurrence of debris discs around main-sequence A and G stars
Debris discs consist of large dust grains that are generated bycollisions of comets or asteroids around main-sequence stars, and thequantity and distribution of debris may be used to detect the presenceof perturbing planets akin to Neptune. We use stellar and disc surveysto compare the material seen around A- and G-type main-sequence stars.Debris is detected much more commonly towards A stars, even when acomparison is made only with G stars of comparable age. Detection ratesare consistent with disc durations of ~0.5 Gyr, which may occur at anytime during the main sequence. The higher detection rate for A stars canresult from this duration being a larger fraction of the main-sequencelifetime, possibly boosted by a globally slightly larger disc mass thanfor the G-type counterparts. The disc mass range at any given age is afactor of at least ~100 and any systematic decline with time is slow,with a power law estimated to not be steeper than t-1/2.Comparison with models shows that dust can be expected as late as a fewGyr when perturbing planetesimals form slowly at large orbital radii.Currently, the Solar system has little dust because the radius of theKuiper Belt is small and hence the time-scale to produce planetesimalswas less than 1 Gyr. However, the apparently constant duration of ~0.5Gyr when dust is visible is not predicted by the models.
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.
We have embarked on a project, under the aegis of the Nearby Stars(NStars)/Space Interferometry Mission Preparatory Science Program, toobtain spectra, spectral types, and, where feasible, basic physicalparameters for the 3600 dwarf and giant stars earlier than M0 within 40pc of the Sun. In this paper, we report on the results of this projectfor the first 664 stars in the northern hemisphere. These resultsinclude precise, homogeneous spectral types, basic physical parameters(including the effective temperature, surface gravity, and overallmetallicity [M/H]), and measures of the chromospheric activity of ourprogram stars. Observed and derived data presented in this paper arealso available on the project's Web site.
| Dependence of coronal X-ray emission on spot-induced brightness variations in cool main sequence stars
The maximum amplitude (Amax) of spot-induced brightnessvariations from long-term V-band photometry and the ratioLX/Lbol between X-ray and bolometric luminositiesare suitable indicators of the level of magnetic activity in thephotosphere and in the corona of late-type stars, respectively. By usingthese activity indicators we investigate the dependence of coronal X-rayemission on the level of photospheric starspot activity in a homogeneoussample of low mass main sequence field and cluster stars of differentages (IC 2602, IC 4665,IC 2391, alpha Persei,Pleiades and Hyades). First, theactivity-rotation connection at the photospheric level is re-analysed,as well as its dependence on spectral type and age. The upper envelopeof Amax increases monotonically with decreasing rotationalperiod (P) and Rossby number (R0) showing a break around 1.1d that separates two rotation regimes where the starspot activity showsdifferent behaviours. The Amax-P andAmax-R0 relations are fitted with linear,exponential and power laws to look for the function which bestrepresents the trend of the data. The highest values of Amaxare found among K-type stars and at the ages of alphaPersei and Pleiades. We also analyse theactivity-rotation connection at the coronal level as well as itsdependence on spectral type. The level of X-ray emission increases withincreasing rotation rate up to a saturation level. The rotational periodat which saturation occurs is colour-dependent and increases withadvancing spectral type. Also the LX/Lbol-P andLX/Lbol-R0 relations are fitted withlinear, exponential and power laws to look for the best fittingfunction. Among the fastest rotating stars (P<=0.3 d) there isevidence of super-saturation. Also the highest values ofLXLbol are found among K-type stars. Finally, thephotospheric-coronal activity connection is investigated by using forthe first time the largest ever sample of light curve amplitudes asindicators of the magnetic filling factor. The activity parametersLX/Lbol and Amax are found to becorrelated with each other, thus confirming the dependence of coronalactivity on photospheric magnetic fields. More precisely, theLX/Lbol-Amax distribution shows thepresence of an upper envelope, which is constant at theLX/Lbol =~ -3.0 saturation level, and of a lowerenvelope. The best fit to the lower envelope is given by a power lawwith steepness decreasing from F-G to M spectral types. However, it isconsidered a tentative result, since the fit reduced chi-squares arelarge. Such spectral-type dependence may be related to a colourdependence of Amax on the total starspot filling factor, aswell as to the coronal emission being possibly more sensitive tostarspot activity variations in F- and G-type than in M-type stars. TheLX/Lbol-Amax mean values for eachcluster in our sample decrease monotonically with increasing age,showing that the levels of photospheric and coronal activity evolve intime according to a single power law till the Sun's age.Tables of the photometric and X-ray data sets are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/410/671
| Multiplicity among solar-type stars. III. Statistical properties of the F7-K binaries with periods up to 10 years
Two CORAVEL radial velocity surveys - one among stars in the solarneighbourhood, the other in the Pleiades and in Praesepe - are merged toderive the statistical properties of main-sequence binaries withspectral types F7 to K and with periods up to 10 years. A sample of 89spectroscopic orbits was finally obtained. Among them, 52 relate to afree-of-bias selection of 405 stars (240 field stars and 165 clusterstars). The statistics corrected for selection effects yield thefollowing results: (1) No discrepancy is found between the binariesamong field stars and the binaries in open cluster. The distributions ofmass ratios, of periods, the period-eccentricity diagram and the binaryfrequencies are all within the same error intervals. (2) Thedistribution of mass ratios presents two maxima: a broad peak from q ~0.2 to q ~ 0.7, and a sharp peak for q > 0.8 (twins). Both arepresent among the early-type as well as among the late-type part of thesample, indicating a scale-free formation process. The peak for q >0.8 gradually decreases when long-period binaries are considered.Whatever their periods, the twins have eccentricities significantlylower than the other binaries, confirming a difference in the formationprocesses. Twins could be generated by in situ formation followed byaccretion from a gaseous envelope, whereas binaries with intermediatemass ratios could be formed at wide separations, but they are madecloser by migration led by interactions with a circumbinary disk. (3)The frequency of binaries with P<10 years is about 14%. (4) About0.3% of binaries are expected to appear as false positives in a planetsearch. Therefore, the frequency of planetary systems among stars ispresently 7+4-2%. The extension of thedistribution of mass ratios in the planetary range would result in avery sharp and very high peak, well separated from the binary stars withlow mass ratios. Based on photoelectric radial-velocity measurementscollected at Haute-Provence observatory and on observations made withthe ESA Hipparcos astrometry satellite.
| The stellar activity-rotation relationship revisited: Dependence of saturated and non-saturated X-ray emission regimes on stellar mass for late-type dwarfs
We present the results of a new study on the relationship betweencoronal X-ray emission and stellar rotation in late-type main-sequencestars. We have selected a sample of 259 dwarfs in the B-V range 0.5-2.0,including 110 field stars and 149 members of the Pleiades, Hyades, alphaPersei, IC 2602 and IC 2391 open clusters. All the stars have beenobserved with ROSAT, and most of them have photometrically-measuredrotation periods available. Our results confirm that two emissionregimes exist, one in which the rotation period is a good predictor ofthe total X-ray luminosity, and the other in which a constant saturatedX-ray to bolometric luminosity ratio is attained; we present aquantitative estimate of the critical rotation periods below which starsof different masses (or spectral types) enter the saturated regime. Inthis work we have also empirically derived a characteristic time scale,taue , which we have used to investigate the relationshipbetween the X-ray emission level and an X-ray-based Rossby numberRe = Prot/taue: we show that ourempirical time scale taue resembles the theoreticalconvective turnover time for 0.4 <~ M/Msun <~ 1.2, butit also has the same functional dependence on B-V asLbol-1/2 in the color range 0.5 <~ B-V <~1.5. Our results imply that - for non-saturated coronae - theLx - Prot relation is equivalent to theLx/Lbol vs. Re relation. Tables 1 and 2are only available in electronic form at \ http://www.edpsciences.org
| 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
| CHARM: A Catalog of High Angular Resolution Measurements
The Catalog of High Angular Resolution Measurements (CHARM) includesmost of the measurements obtained by the techniques of lunaroccultations and long-baseline interferometry at visual and infraredwavelengths, which have appeared in the literature or have otherwisebeen made public until mid-2001. A total of 2432 measurements of 1625sources are included, along with extensive auxiliary information. Inparticular, visual and infrared photometry is included for almost allthe sources. This has been partly extracted from currently availablecatalogs, and partly obtained specifically for CHARM. The main aim is toprovide a compilation of sources which could be used as calibrators orfor science verification purposes by the new generation of largeground-based facilities such as the ESO Very Large Interferometer andthe Keck Interferometer. The Catalog is available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/386/492, and from theauthors on CD-Rom.
| Chromospherically young, kinematically old stars
We have investigated a group of stars known to have low chromosphericages, but high kinematical ages. Isochrone, chemical and lithium agesare estimated for them. The majority of stars in this group show lithiumabundances much smaller than expected for their chromospheric ages,which is interpreted as an indication of their old age. Radial velocitymeasurements in the literature also show that they are not closebinaries. The results suggest that they can be formed from thecoalescence of short-period binaries. Coalescence rates, calculatedtaking into account several observational data and a maximum theoreticaltime scale for contact, in a short-period pair, predict a number ofcoalesced stars similar to what we have found in the solarneighbourhood.
| Late-type members of young stellar kinematic groups - I. Single stars
This is the first paper of a series aimed at studying the properties oflate-type members of young stellar kinematic groups. We concentrate ourstudy on classical young moving groups such as the Local Association(Pleiades moving group, 20-150Myr), IC 2391 supercluster (35Myr), UrsaMajor group (Sirius supercluster, 300Myr), and Hyades supercluster(600Myr), as well as on recently identified groups such as the Castormoving group (200Myr). In this paper we compile a preliminary list ofsingle late-type possible members of some of these young stellarkinematic groups. Stars are selected from previously established membersof stellar kinematic groups based on photometric and kinematicproperties as well as from candidates based on other criteria such astheir level of chromospheric activity, rotation rate and lithiumabundance. Precise measurements of proper motions and parallaxes takenfrom the Hipparcos Catalogue, as well as from the Tycho-2 Catalogue, andpublished radial velocity measurements are used to calculate theGalactic space motions (U, V, W) and to apply Eggen's kinematic criteriain order to determine the membership of the selected stars to thedifferent groups. Additional criteria using age-dating methods forlate-type stars will be applied in forthcoming papers of this series. Afurther study of the list of stars compiled here could lead to a betterunderstanding of the chromospheric activity and their age evolution, aswell as of the star formation history in the solar neighbourhood. Inaddition, these stars are also potential search targets for directimaging detection of substellar companions.
| A revision of the solar neighbourhood metallicity distribution
We present a revised metallicity distribution of dwarfs in the solarneighbourhood. This distribution is centred on solar metallicity. Weshow that previous metallicity distributions, selected on the basis ofspectral type, are biased against stars with solar metallicity orhigher. A selection of G-dwarf stars is inherently biased againstmetal-rich stars and is not representative of the solar neighbourhoodmetallicity distribution. Using a sample selected on colour, we obtain adistribution where approximately half the stars in the solarneighbourhood have metallicities higher than [Fe/H]=0. The percentage ofmid-metal-poor stars ([Fe/H]<-0.5) is approximately 4 per cent, inagreement with present estimates of the thick disc. In order to have ametallicity distribution comparable to chemical evolution modelpredictions, we convert the star fraction to mass fraction, and showthat another bias against metal-rich stars affects dwarf metallicitydistributions, due to the colour (or spectral type) limits of thesamples. Reconsidering the corrections resulting from the increasingthickness of the stellar disc with age, we show that the simpleclosed-box model with no instantaneous recycling approximation gives areasonable fit to the observed distribution. Comparisons with theage-metallicity relation and abundance ratios suggest that the simpleclosed-box model may be a viable model of the chemical evolution of theGalaxy at solar radius.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| The ``rotation-activity connection'': Its extension to photospheric activity diagnostics
In this paper we present the results of a different approach in thestudy of the so-called rotation-activity connection, which is a wellestablished correlation between rotation and magnetic activity atchromospheric and outer atmospheric levels. The present study concernsthe photospheric level and was carried out by using V-band photometriclight curve amplitudes as indicators of starspot coverage and ofmagnetic activity. A high degree of correlation between the envelope ofmaximum V-band light curve amplitudes and the rotation period is foundfor the active star members of young open clusters (IC 2602, IC 2391,Alpha Persei, Pleiades and Hyades), as well as for active field stars.This correlation shows a different behaviour in two different rotationperiod ranges. Moreover, some evidence of a possible activity``saturation'' is found among the most rapidly rotating stars of thesample. Additional correlations between photospheric and other magneticactivity indicators in the chromosphere, transition region and coronaare also investigated. The results presented here can be considered asan extension of the well established rotation-activity connection validfrom the corona, transition region and chromosphere, down to thephotosphere.
| A spectroscopic study of the eclipsing binaries SV Camelopardalis and XY Ursae Majoris
High-resolution spectroscopic observations of the eclipsing RS CVn-typeactive close binaries SV Camelopardalis and XY Ursae Majoris revealexcess emission components in the Hα and Hβ lines. We haveused the spectral subtraction technique to separate the excess emissionfrom the photospheric background and find that in both stars the excessemission is associated with the secondary, cooler component. Analysis ofthe EWHα/EWHβ ratio indicates that inboth cases the emission is probably associated with surface plageregions or prominences viewed against the stellar disks. We find noevidence of excess absorption features associated with extendedprominence-like material in these systems. Based on observations made atObservatoire de Haute Provence (CNRS), France.
| Photometric Measurements of the Fields of More than 700 Nearby Stars
In preparation for optical/IR interferometric searches for substellarcompanions of nearby stars, we undertook to characterize the fields ofall nearby stars visible from the Northern Hemisphere to determinesuitable companions for interferometric phase referencing. Because theKeck Interferometer in particular will be able to phase-reference oncompanions within the isoplanatic patch (30") to about 17th magnitude atK, we took images at V, r, and i that were deep enough to determine iffield stars were present to this magnitude around nearby stars using aspot-coated CCD. We report on 733 fields containing 10,629 measurementsin up to three filters (Gunn i, r and Johnson V) of nearby stars down toabout 13th magnitude at V.
| The ROSAT all-sky survey catalogue of the nearby stars
We present X-ray data for all entries of the Third Catalogue of NearbyStars \cite[(Gliese & Jahreiss 1991)]{gli91} that have been detectedas X-ray sources in the ROSAT all-sky survey. The catalogue contains1252 entries yielding an average detection rate of 32.9 percent. Inaddition to count rates, source detection parameters, hardness ratios,and X-ray fluxes we also list X-ray luminosities derived from Hipparcosparallaxes. Catalogue also available at CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Measurements of magnetic field strength on T Tauri stars
We have investigated the magnetic field strength of one weak-line andfour classical T Tauri stars. The magnetic field strength is derivedfrom the differential change of the equivalent width of photospheric FeI lines in the presence of a magnetic field, calculated using a fullradiative transfer code. The method was successfully tested by applyingit to a non-magnetic solar-type star, and to VY Ariwhich is believed to have a strong magnetic field. For two of theclassical T Tauri stars, we find a product of magnetic field strengthand filling factor B * f = (2.35+/- 0.15) kG for TTau, and B * f = (1.1+/- 0.2) kG for LkCa15. For the classical T Tauri star UX Tau Aand the weak-line T Tauri star LkCa 16 the detectionis only marginal, indicating magnetic field strengths of the order of 1kG and possibly of more than 2 kG, respectively. No field could bedetected for the classical T Tauri star GW Ori. Forthe two classical T Tauri stars for which we have detected a field, wefind the filling factors to be larger than ~ 0.5, which indicates thatthe magnetic field covers most of the photosphere. We also show thatignoring a magnetic field can, depending on the lines used, result inerrors in effective temperature and underestimates of veiling. Based onobservations made with the William Herschel Telescope operated on theisland of La Palma by the Royal Greenwich Observatory in the SpanishObservatorio de los Roque de los Muchachos of the Instituto deAstrofisica de Canarias
| Nearby Young Solar Analogs. I. Catalog and Stellar Characteristics
We present a catalog of 38 young solar analogs within 25 pc, stars thatare uniquely well suited for observations of their circumstellarenvironments to improve our understanding of conditions within the solarsystem during the Hadean/early Archean eons (prior to 3.8 Gyr ago).These G and early K stars were selected from the Hipparcos astrometriccatalog based on lack of known stellar companions within 800 AU,bolometric luminosities close to that of the zero-age Sun and consistentwith the zero-age main sequence, and ROSAT X-ray luminositiescommensurate with the higher rotation rate and level of dynamo-drivenactivity in solar-mass stars less than 0.8 Gyr old. While many of theseobjects have been previously identified, this sample is novel in tworespects: The selection criteria specifically consider the planetaryenvironment, and the selection is uniform and all-sky. The X-rayemission from these young analogs is spectrally soft and consistent witha coronal origin. Calcium H and K emission, rotation periods, lithiumabundances, and kinematics support an age range of 0.2-0.8 Gyr for mostof these stars. Three stars have exceptionally high space motions withrespect to the local standard of rest and may be old disk or halo starsthat are anomalously X-ray luminous.
| Latitude distributions and lifetimes of star-spots on G dwarfs in the alpha Persei cluster
We present a set of maximum-entropy reconstructions of the star-spotdistributions on two rapidly rotating G dwarfs in the alpha Perseicluster, from spectra taken at the William Herschel Telescope on threenights in 1996 October and November. Since these stars are too faint forconventional Doppler imaging, which makes use of only one or a fewlines, we take the large number of photospheric metal lines available inan echelle spectrum, and deconvolve them into a single, highsignal-to-noise ratio profile. We show that this technique results in atypical multiplex gain of 22.5 in signal-to-noise ratio for a givenspectrum, the equivalent of using a single line obtained on a 63-mtelescope. The image reconstructions demonstrate that both these starshave cool high-latitude regions or polar crowns, and low-latitudefeatures, in contradiction to the suggestion that only high-latitudespots should be present. Cross-correlation between image reconstructionsof He 699, 31 days apart, reveals a lack of correlation between detailedsmall-scale structures. This places an upper limit for the lifetime ofthe observed features at less than one month. The Hα profiles arealso found to exhibit absorption features indicating the presence ofprominence clouds, at or below the corotation radius.
| Metallicity effects on the chromospheric activity-age relation for late-type dwarfs
We show that there is a relationship between the age excess, defined asthe difference between the stellar isochrone and chromospheric ages, andthe metallicity as measured by the index [Fe/H] for late-type dwarfs.The chromospheric age tends to be lower than the isochrone age formetal-poor stars, and the opposite occurs for metal-rich objects. Wesuggest that this could be an effect of neglecting the metallicitydependence of the calibrated chromospheric emission-age relation. Wepropose a correction to account for this dependence. We also investigatethe metallicity distributions of these stars, and show that there aredistinct trends according to the chromospheric activity level. Inactivestars have a metallicity distribution which resembles the metallicitydistribution of solar neighbourhood stars, while active stars appear tobe concentrated in an activity strip on the logR'_HKx[Fe/H] diagram. Weprovide some explanations for these trends, and show that thechromospheric emission-age relation probably has different slopes on thetwo sides of the Vaughan-Preston gap.
| Surface inhomogeneities and line variability on DF Tau
We have mapped surface inhomogeneities on the classical T Tauri star DFTau, using the Lii doublet at 670.8 nm, the Cai lines at 612.2 nm and643.9 nm and a calcium and iron blend at 646.3 nm. We find compellingevidence that there are hotspots with temperatures of more than 5000 K.Two of the hotspots produce line-profile deformations that can be tracedas they move through the cross-correlated profiles. When one of thehotspots crosses the stellar disc, redshifted absorption componentsappear in the Na D lines. As these redshifted absorption features areusually tracers for mass-infall we interpret this hotspot as anaccretion shock close to the stellar surface. Parts of the surface of DFTau are covered with a hot chromosphere that is visible in the Caiiinfrared triplet lines and the narrow component of Hei. We find nocorrelation between the veiling and the lines that originate from thehot chromosphere, suggesting that the veiling and the chromosphericemission are produced in physically distinct regions.
| FU Orionis Resolved by Infrared Long-Baseline Interferometry at a 2 AU Scale
We present the first infrared interferometric observations of a youngstellar object with a spatial projected resolution better than 2 AU. Theobservations were obtained with the Palomar Testbed Interferometer(PTI). FU Orionis exhibits a visibility of V^2=0.72+/-0.07 for a 103+/-5m-projected baseline at lambda=2.2 mum. On the spatial scale probed bythe PTI, the data are consistent with both a binary system scenario (amaximum magnitude difference of 2.7+/-0.5 mag and the smallestseparation of 0.35+/-0.05 AU) and a standard luminous accretion diskmodel (M~6x10^-5 M_solar yr^-1), where the thermal emission dominatesthe stellar scattering, and are inconsistent with a single stellarphotosphere.
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Observation and Astrometry data
| Constellation: | オリオン座 |
| Right ascension: | 06h13m12.60s |
| Declination: | +10°37'39.0" |
| Apparent magnitude: | 6.45 |
| Distance: | 18.116 parsecs |
| Proper motion RA: | 77.3 |
| Proper motion Dec: | -297.3 |
| B-T magnitude: | 7.241 |
| V-T magnitude: | 6.499 |
Catalogs and designations:
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