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Potential Members of Stellar Kinematic Groups within 30 pc of the Sun
We analyze the kinematic histories of stars within 30 pc of the Sun, forwhich three-dimensional spatial coordinates and three-dimensionalvelocity vectors are available. From this sample, we extract members ofstellar kinematic groups (SKGs) in the following manner. First, weconsider in the three-dimensional velocity space centered on the localstandard of rest, a sphere with a radius of 8 km s-1centered on the mean velocity vector of a particular SKG. Around eachSKG velocity center, we have found a significant excess of starscompared to background field stars. For each candidate, in thethree-dimensional spatial coordinate space, its trajectory is tracedback in time by the age of the relevant SKG to obtain the estimateddistance from the SKG center at the time of the SKG's birth by theepicyclic approximation and harmonic vertical motion. It often happensthat a star is a candidate member of multiple SKGs. Then we rank thecandidacy to multiple SKGs based on the smallness of distanceseparations. In this manner, we have kinematically selected 238candidates. We further impose at least one of the following qualitativecriteria for being a member: spectral type A or B, variability, or EUVand X-ray emission. We have finally selected 137 candidate members ofSKGs out of a sample of 966 stars.
| Potential Members of Stellar Kinematical Groups within 20 pc of the Sun
We analyze the kinematical histories of stars within 20 pc of the Sun,for which three-dimensional spatial coordinates and three-dimensionalvelocity vectors are available. From this sample, we extract members ofstellar kinematical groups (SKGs) in the following manner. First, in thethree-dimensional velocity space centered on the local standard of rest,we consider a sphere with a radius of 8 km s-1 centeredon the mean velocity vector of a particular SKG. Around each SKGvelocity center, we have found a significant excess of stars compared tobackground stars. For each candidate, in the three-dimensional spatialcoordinate space, its trajectory is traced back in time by the age ofthe relevant SKG, to estimate the distance from the SKG center at thetime of the SKG's birth by the epicycle approximation and verticalharmonic motion. It often happens that a star is a candidate member ofmultiple SKGs. Then we rank the candidacy to multiple SKGs based on thesmallness of distance separations. In this manner, we have kinematicallyselected 74 candidate members of SKGs out of a sample of 383 stars. Ifwe take into account stellar properties, the number is reduced to 68.
| Reaching the boundary between stellar kinematic groups and very wide binaries . II. ? Librae + KU Librae: a common proper motion system in Castor separated by 1.0 pc
Aims: I investigate the gravitational binding of a nearby commonproper motion system in the young Castor moving group (? ~ 200 Ma),which is formed by the bright quadruple star ? Lib (Zubenelgenubi)and the young solar analogue KU Lib. The system has an exceptionallywide angular separation of about 2.6 deg, which corresponds to aprojected physical separation of about 1.0 pc. Methods: Icompiled basic information on the system, compared its binding energywith those of other weakly bound systems in the field, and studied thephysical separations of resolved multiple systems in Castor. Results: KU Lib has roughly the same proper motion, parallacticdistance, radial velocity, and metallicity as the young hierarchicalquadruple system ? Lib. It also displays youth features. Theresemblance between these basic parameters and the relatively highestimated binding energy indicate that the five stars aregravitationally bound. KU Lib and ? Lib constitute the widestknown multiple system in all mass domains, and probably represent themost extreme example of young wide binaries on the point of beingdisrupted. Besides this, I make a comprehensive compilation of starcandidates in Castor, including new ones.
| Imaging Young Giant Planets From Ground and Space
High-contrast imaging can find and characterize gas giant planets aroundnearby young stars and the closest M stars, complementing radialvelocity and astrometric searches by exploring orbital separationsinaccessible to indirect methods. Ground-based coronagraphs are alreadyprobing within 25 AU of nearby young stars to find objects as small as .This paper contrasts near-term and future ground-based capabilities withhigh-contrast imaging modes of the James Webb Space Telescope (JWST).Monte Carlo modeling reveals that JWST can detect planets with masses assmall as across a broad range of orbital separations. We present newcalculations for planet brightness as a function of mass and age forspecific JWST filters and extending to .
| Rotational Velocities for M Dwarfs
We present spectroscopic rotation velocities (v sin i) for 56 M dwarfstars using high-resolution Hobby-Eberly Telescope High ResolutionSpectrograph red spectroscopy. In addition, we have also determinedphotometric effective temperatures, masses, and metallicities ([Fe/H])for some stars observed here and in the literature where we couldacquire accurate parallax measurements and relevant photometry. We haveincreased the number of known v sin i values for mid M stars by around80% and can confirm a weakly increasing rotation velocity withdecreasing effective temperature. Our sample of v sin is peak at lowvelocities (~3 km s-1). We find a change in therotational velocity distribution between early M and late M stars, whichis likely due to the changing field topology between partially and fullyconvective stars. There is also a possible further change in therotational distribution toward the late M dwarfs where dust begins toplay a role in the stellar atmospheres. We also link v sin i to age andshow how it can be used to provide mid-M star age limits. When allliterature velocities for M dwarfs are added to our sample, there are198 with v sin i <= 10 km s-1 and 124 in themid-to-late M star regime (M3.0-M9.5) where measuring precision opticalradial velocities is difficult. In addition, we also search the spectrafor any significant Hα emission or absorption. Forty three percentwere found to exhibit such emission and could represent young, activeobjects with high levels of radial-velocity noise. We acquired twoepochs of spectra for the star GJ1253 spread by almost one month and theHα profile changed from showing no clear signs of emission, toexhibiting a clear emission peak. Four stars in our sample appear to below-mass binaries (GJ1080, GJ3129, Gl802, and LHS3080), with both GJ3129and Gl802 exhibiting double Hα emission features. The tablespresented here will aid any future M star planet search target selectionto extract stars with low v sin i.Based on observations obtained with the Hobby-Eberly Telescope, which isa joint project of the University of Texas at Austin, the PennsylvaniaState University, Stanford University,Ludwig-Maximilians-Universität München, andGeorg-August-Universität Göttingen.
| χ Values for Blue Emission Lines in M Dwarfs
We compute values for blue emission lines in active M dwarfs. Usingflux-calibrated spectra from nearby M dwarfs and spectral M dwarftemplates from SDSS, we derive analytical relations that describe howthe values for the Ca II H and K as well as the Hβ, Hγ,Hδ, Hɛ, and H8 Balmer emission lines vary as a function ofspectral type and color. These derived values are important for numerousM dwarf studies where the intrinsic luminosity of emission lines cannotbe estimated due to uncertain distances and/or non-flux-calibratedspectra. We use these results to estimate the mean properties of blueemission lines in active-field M dwarfs from SDSS.
| New Distant Companions to Known Nearby Stars. II. Faint Companions of Hipparcos Stars and the Frequency of Wide Binary Systems
We perform a search for faint, common proper motion companions ofHipparcos stars using the recently published Lépine-Shara ProperMotion-North catalog of stars with proper motionμ>0.15'' yr-1. Our survey uncovers a totalof 521 systems with angular separations3''<Δθ<1500'', with 15 triplesand 1 quadruple. Our new list of wide systems with Hipparcos primariesincludes 130 systems identified here for the first time, including 44 inwhich the secondary star has V>15.0. Our census is statisticallycomplete for secondaries with angular separations20''<Δθ<300'' and apparentmagnitudes V<19.0. Overall, we find that at least 9.5% of nearby(d<100 pc) Hipparcos stars have distant stellar companions withprojected orbital separations s>1000 AU. We observe that thedistribution in orbital separations is consistent with Öpik's law,f(s)ds~s-1ds, only up to a separation s~4000 AU, beyond whichit follows a more steeply decreasing power law f(s)ds~s-ldswith l=1.6+/-0.1. We also find that the luminosity function of thesecondaries is significantly different from that of the single stars'field population, showing a relative deficiency in low-luminosity(8
| Proper-motion binaries in the Hipparcos catalogue. Comparison with radial velocity data
Context: .This paper is the last in a series devoted to the analysis ofthe binary content of the Hipparcos Catalogue. Aims: .Thecomparison of the proper motions constructed from positions spanning ashort (Hipparcos) or long time (Tycho-2) makes it possible to uncoverbinaries with periods of the order of or somewhat larger than the shorttime span (in this case, the 3 yr duration of the Hipparcos mission),since the unrecognised orbital motion will then add to the propermotion. Methods: .A list of candidate proper motion binaries isconstructed from a carefully designed χ2 test evaluatingthe statistical significance of the difference between the Tycho-2 andHipparcos proper motions for 103 134 stars in common between the twocatalogues (excluding components of visual systems). Since similar listsof proper-motion binaries have already been constructed, the presentpaper focuses on the evaluation of the detection efficiency ofproper-motion binaries, using different kinds of control data (mostlyradial velocities). The detection rate for entries from the NinthCatalogue of Spectroscopic Binary Orbits (S_B^9) is evaluated, as wellas for stars like barium stars, which are known to be all binaries, andfinally for spectroscopic binaries identified from radial velocity datain the Geneva-Copenhagen survey of F and G dwarfs in the solarneighbourhood. Results: .Proper motion binaries are efficientlydetected for systems with parallaxes in excess of ~20 mas, and periodsin the range 1000-30 000 d. The shortest periods in this range(1000-2000 d, i.e., once to twice the duration of the Hipparcos mission)may appear only as DMSA/G binaries (accelerated proper motion in theHipparcos Double and Multiple System Annex). Proper motion binariesdetected among S_B9 systems having periods shorter than about400 d hint at triple systems, the proper-motion binary involving acomponent with a longer orbital period. A list of 19 candidate triplesystems is provided. Binaries suspected of having low-mass(brown-dwarf-like) companions are listed as well. Among the 37 bariumstars with parallaxes larger than 5 mas, only 7 exhibit no evidence forduplicity whatsoever (be it spectroscopic or astrometric). Finally, thefraction of proper-motion binaries shows no significant variation amongthe various (regular) spectral classes, when due account is taken forthe detection biases.Full Table [see full textsee full text] is 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/464/377
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Statistical Constraints for Astrometric Binaries with Nonlinear Motion
Useful constraints on the orbits and mass ratios of astrometric binariesin the Hipparcos catalog are derived from the measured proper motiondifferences of Hipparcos and Tycho-2 (Δμ), accelerations ofproper motions (μ˙), and second derivatives of proper motions(μ̈). It is shown how, in some cases, statistical bounds can beestimated for the masses of the secondary components. Two catalogs ofastrometric binaries are generated, one of binaries with significantproper motion differences and the other of binaries with significantaccelerations of their proper motions. Mathematical relations betweenthe astrometric observables Δμ, μ˙, and μ̈ andthe orbital elements are derived in the appendices. We find a remarkabledifference between the distribution of spectral types of stars withlarge accelerations but small proper motion differences and that ofstars with large proper motion differences but insignificantaccelerations. The spectral type distribution for the former sample ofbinaries is the same as the general distribution of all stars in theHipparcos catalog, whereas the latter sample is clearly dominated bysolar-type stars, with an obvious dearth of blue stars. We point outthat the latter set includes mostly binaries with long periods (longerthan about 6 yr).
| A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)
The LSPM catalog is a comprehensive list of 61,977 stars north of theJ2000 celestial equator that have proper motions larger than 0.15"yr-1 (local-background-stars frame). The catalog has beengenerated primarily as a result of our systematic search for high propermotion stars in the Digitized Sky Surveys using our SUPERBLINK software.At brighter magnitudes, the catalog incorporates stars and data from theTycho-2 Catalogue and also, to a lesser extent, from the All-SkyCompiled Catalogue of 2.5 million stars. The LSPM catalog considerablyexpands over the old Luyten (Luyten Half-Second [LHS] and New LuytenTwo-Tenths [NLTT]) catalogs, superseding them for northern declinations.Positions are given with an accuracy of <~100 mas at the 2000.0epoch, and absolute proper motions are given with an accuracy of ~8 masyr-1. Corrections to the local-background-stars propermotions have been calculated, and absolute proper motions in theextragalactic frame are given. Whenever available, we also give opticalBT and VT magnitudes (from Tycho-2, ASCC-2.5),photographic BJ, RF, and IN magnitudes(from USNO-B1 catalog), and infrared J, H, and Ks magnitudes(from 2MASS). We also provide an estimated V magnitude and V-J color fornearly all catalog entries, useful for initial classification of thestars. The catalog is estimated to be over 99% complete at high Galacticlatitudes (|b|>15deg) and over 90% complete at lowGalactic latitudes (|b|>15deg), down to a magnitudeV=19.0, and has a limiting magnitude V=21.0. All the northern starslisted in the LHS and NLTT catalogs have been reidentified, and theirpositions, proper motions, and magnitudes reevaluated. The catalog alsolists a large number of completely new objects, which promise to expandvery significantly the census of red dwarfs, subdwarfs, and white dwarfsin the vicinity of the Sun.Based on data mining of the Digitized Sky Surveys (DSSs), developed andoperated by the Catalogs and Surveys Branch of the Space TelescopeScience Institute (STScI), Baltimore.Developed with support from the National Science Foundation (NSF), aspart of the NASA/NSF NStars program.
| New neighbours. III. 21 new companions to nearby dwarfs, discovered with adaptive optics
We present some results of a CFHT adaptive optics search for companionsto nearby dwarfs. We identify 21 new components in solar neighbourhoodsystems, of which 13 were found while surveying a volume-limited sampleof M dwarfs within 12 pc. We are obtaining complete observations forthis subsample, to derive unbiased multiplicity statistics for thevery-low-mass disk population. Additionally, we resolve for the firsttime 6 known spectroscopic or astrometric binaries, for a total of 27newly resolved companions. A significant fraction of the new binarieshas favourable parameters for accurate mass determinations. The newlyresolved companion of Gl 120.1C was thought to have a spectroscopicminimum mass in the brown-dwarf range (Duquennoy & Mayor\cite{duquennoy91}), and it contributed to the statistical evidence thata few percent of solar-type stars might have close-in brown-dwarfcompanions. We find that Gl 120.1C actually is an unrecogniseddouble-lined spectroscopic pair. Its radial-velocity amplitude hadtherefore been strongly underestimated by Duquennoy & Mayor(\cite{duquennoy91}), and it does not truly belong to their sample ofsingle-lined systems with minimum spectroscopic mass below thesubstellar limit. We also present the first direct detection of Gl494B, an astrometric brown-dwarf candidate. Its luminosity straddles thesubstellar limit, and it is a brown dwarf if its age is less than300 Myr. A few more years of observations will ascertain its massand status from first principles.Based on observations made at Canada-France-Hawaii Telescope, operatedby the National Research Council of Canada, the Centre National de laRecherche Scientifique de France and the University of Hawaii. Some ofthe data presented herein were obtained at the W. M. Keck Observatory,which is operated as a scientific partnership among the CaliforniaInstitute of Technology, the University of California and the NationalAeronautics and Space Administration. The Observatory was made possibleby the generous financial support of the W. M. Keck Foundation.
| New Hipparcos-based Parallaxes for 424 Faint Stars
We present a catalog of 424 common proper-motion companions to Hipparcosstars with good (>3 σ) parallaxes, thereby effectively providingnew parallaxes for these companions. Compared with typical stars in theHipparcos catalog, these stars are substantially dimmer. The catalogincludes 20 white dwarfs and an additional 29 stars withMV>14, the great majority of the latter being M dwarfs.
| 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.
| Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is onlyavailable 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/qcat?J/A+A/397/997
| The Palomar/MSU Nearby Star Spectroscopic Survey. III. Chromospheric Activity, M Dwarf Ages, and the Local Star Formation History
We present high-resolution echelle spectroscopy of 676 nearby M dwarfs.Our measurements include radial velocities, equivalent widths ofimportant chromospheric emission lines, and rotational velocities forrapidly rotating stars. We identify several distinct groups by theirHα properties and investigate variations in chromospheric activityamong early (M0-M2.5) and mid (M3-M6) dwarfs. Using a volume-limitedsample together with a relationship between age and chromosphericactivity, we show that the rate of star formation in the immediate solarneighborhood has been relatively constant over the last 4 Gyr. Inparticular, our results are inconsistent with recent large bursts ofstar formation. We use the correlation between Hα activity and ageas a function of color to set constraints on the properties of L and Tdwarf secondary components in binary systems. We also identify a numberof interesting stars, including rapid rotators, radial velocityvariables, and spectroscopic binaries. Observations were made at the 60inch telescope at Palomar Mountain, which is jointly owned by theCalifornia Institute of Technology and the Carnegie Institution ofWashington.
| Meeting the Cool Neighbors. I. Nearby Stars in the NLTT Catalogue: Defining the Sample
We are currently undertaking a program aimed at identifying previouslyunrecognized late-type dwarfs within 20 pc of the Sun. As a first step,we have cross-referenced Luyten's NLTT proper-motion catalog against thesecond incremental release of the Two Micron All Sky Survey (2MASS)Point Source Catalog and use optical/infrared colors, derived bycombining Luyten's mr estimates with 2MASS data, to identifycandidate nearby stars. This paper describes the definition of areference sample of 1245 stars and presents a compilation of literaturedata for more than one-third of the sample. Only 274 stars havetrigonometric parallax measurements, but we have used data for nearbystars with well-determined trigonometric parallaxes to computecolor-magnitude relations in the (MV, V-K), (MV,V-I), and (MI, I-J) planes and use those relations todetermine photometric parallaxes for NLTT stars with optical photometry.Based on the 2MASS JHKs data alone, we have identified afurther 42 ultracool dwarfs (J-Ks>0.99) and useJ-Ks colors to estimate photometric parallaxes. Combiningthese various techniques, we identify 308 stars with formal distances ofless than 20 pc, while a further 46 have distance estimates within 1σ of our survey limit. Of these 354 stars, 75, including 39 of theultracool dwarfs, are new to nearby-star catalogs. Two stars with bothoptical and near-infrared photometry are potential additions to theimmediate solar neighborhood, with formal distance estimates of lessthan 10 pc.
| 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
| Catalogue and bibliography of the UV Cet-type flare stars and related objects in the solar vicinity
This new catalogue of flare stars includes 463 objects. It containsastrometric, spectral and photometric data as well as information on theinfrared, radio and X-ray properties and general stellar parameters.From the total reference list of about 3400 articles, partial listsselected by objects, authors, key words and by any pairs of thesecriteria can be obtained Tables 1, 2 and 3 are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html.
| 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
| The Galactic Orbits of Nearby UV Ceti Stars
The galactic orbits of 93 UV Ceti stars of the solar neighborhood havebeen numerically integrated. The UV Ceti stars studied are those of theworking list for which Poveda et al. (1996a) determined kinematicproperties and ages. All stars are contained within 25 pc of the Sun(π ≥ 0.04''), and values for their distances, proper motions andradial velocities are available for them (Gliese & Jahreiss 1991).The galactic potential model of Allen & Santillán (1991) wasused, and the orbits were integrated for times similar to the age of theold disk. The galactic orbital parameters are obtained. The orbits areall regular, and the values found for the orbital parameters are similarto those characteristic of the classic young thin disk. The verticalscale height found for the whole sample is 115 pc. However, the orbitalparameters found for the 7 objects with extreme kinematiccharacteristics recognized in Poveda et al. are markedly different fromthose of the rest of the flare stars; in particular, their orbitaleccentricities are larger than 0.3. The vertical scale height of thesample excluding the anomalous objects is just 103 pc. Consequently, wepropose that the anomalous objects belong to the thick disk, which maybe characterized by either e≥ 0.3 or | zmax | > 400 pc.
| EUV activity in late-type stars during the ROSAT WFC All-Sky Survey - II. Comparisons with other observations
The extreme ultraviolet (EUV) observations of the ROSAT Wide FieldCamera All-Sky Survey have revealed bright and energetic coronae for asufficiently large number of main-sequence stars that detailedcomparisons with other observables can be made. We have detected a largenumber of energetic EUV flares on stars of different spectral classes,from dF5 to dM6, including flare stars. The EUV emission iswell-correlated to several stellar properties such as stellar colour,spectral type, bolometric luminosity, far-infrared photosphericemission, etc. These relations are stronger for the highly active starslike flare stars, and they become somewhat looser for the less activedwarfs. We find that there is a better correlation between the EUVluminosity and stellar rotation period for low-activity stars than forhigh-activity ones, and this also applies to the RS CVn stars. This is astrong indication of magnetic/active region saturation in these moreactive stars. We find that there is also a tendency of the L_EUV toincrease with magnetic field intensity, although there are very fewstars with reliable magnetic field strength measurements. These last twocorrelations support the view that the EUV emission from these stars isregulated by magnetic processes. Our results indicate that the stellarcoronae are continuously being heated by small-scale flare events.
| Spectroscopic observations of red dwarfs. III. Observations of red stars in the solar neighborhood.
This list is based on 20 stars in the solar neighborhood for which thereare 52 spectra. Twelve of them are known as UV Ceti flare stars. Theothers behave like flare stars, but are not known to be such. Among the20 there are many binary and triple flare stars. They all belong to thedisk population of the Galaxy. Red dwarfs comprise one of the numerouspopulations of the system. Flare stars either continue to flare or haveceased flare activity. Three diagrams are given that show satisfactoryagreement with the expected ones. A cluster analysis is carried out,which is in agreement with the original proposition and confirms theforegoing.
| EUV activity in late-type stars during the ROSAT WFC All-Sky Survey - I. Techniques and initial results
We study 127 active late-type stars, including the well-known flarestars, in the extreme ultraviolet (EUV) region of the electromagneticspectrum, using the ROSAT Wide Field Camera (WFC) survey observations.Our analysis includes photometry for all the stars in the sample, timinganalysis of the observed photon events, and a statistical analysis forpossible small-scale, low-level variability. 49 stars in our sample weredetected in one or both EUV wavebands. A total of 35 flares were seen,from 23 stars, not all of them well-known flare stars. In addition,about half of the detections exhibited low-level variability. Furtheranalysis reveals that the observed low-level variability was not due torotational or orbital modulation, but rather was related to small-scaleactivity on the stars, possibly in the form of small-amplitude,flare-like events which were too faint to be recognized as individualflares at the sensitivity of the WFC. We call this low-level activity`milliflaring'. We also give estimated upper-limit count rates for thenon-detections.
| The Palomar/MSU Nearby Star Spectroscopic Survey.II.The Southern M Dwarfs and Investigation of Magnetic Activity
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....112.2799H&db_key=AST
| Distribution and Corrlation of Age, Abundance, and Motion of Lower Main Sequence Stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....111..466E&db_key=AST
| Not Available
Not Available
| 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.
| The Palomar/MSU Nearby-Star Spectroscopic Survey. I. The Northern M Dwarfs -Bandstrengths and Kinematics
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....110.1838R&db_key=AST
| Optical identification of EUV sources from the ROSAT Wide Field Camera all-sky survey
Optical identifications for 195 EUV sources located in the ROSAT WideField Camera all-sky survey are presented. We list 69 previously unknownEUV-emitting white dwarfs, 114 active stars, 7 new magnetic cataclysmicvariables and 5 active galaxies. Several of the white dwarfs haveresolved M-type companions, while five are unresolved white dwarf/M-starpairs. Finding charts are given for the optical counterparts.
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| Takýmyýldýz: | Vasak |
| Sað Açýklýk: | 07h31m57.71s |
| Yükselim: | +36°13'09.5" |
| Görünürdeki Parlaklýk: | 10.554 |
| Uzaklýk: | 11.414 parsek |
| özdevim Sað Açýklýk: | -251.9 |
| özdevim Yükselim: | -257.1 |
| B-T magnitude: | 12.507 |
| V-T magnitude: | 10.716 |
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