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Rotation- and temperature-dependence of stellar latitudinal differential rotation
More than 600 high resolution spectra of stars with spectral type F andlater were obtained in order to search for signatures of differentialrotation in line profiles. In 147 stars the rotation law could bemeasured, with 28 of them found to be differentially rotating.Comparison to rotation laws in stars of spectral type A reveals thatdifferential rotation sets in at the convection boundary in theHR-diagram; no star that is significantly hotter than the convectionboundary exhibits the signatures of differential rotation. Four lateA-/early F-type stars close to the convection boundary and at v sin{i}≈ 100 km s-1 show extraordinarily strong absolute shear atshort rotation periods around one day. It is suggested that this is dueto their small convection zone depth and that it is connected to anarrow range in surface velocity; the four stars are very similar inTeff and v sin{i}. Detection frequencies of differentialrotation α = ΔΩ/Ω > 0 were analyzed in starswith varying temperature and rotation velocity. Measurable differentialrotation is more frequent in late-type stars and slow rotators. Thestrength of absolute shear, ΔΩ, and differential rotationα are examined as functions of the stellar effective temperatureand rotation period. The highest values of ΔΩ are found atrotation periods between two and three days. In slower rotators, thestrongest absolute shear at a given rotation rateΔΩmax is given approximately byΔΩmax ∝ P-1, i.e.,αmax ≈ const. In faster rotators, bothαmax and ΔΩmax diminish lessrapidly. A comparison with differential rotation measurements in starsof later spectral type shows that F-stars exhibit stronger shear thancooler stars do and the upper boundary in absolute shear ΔΩwith temperature is consistent with the temperature-scaling law found inDoppler Imaging measurements.
| The relation between X-ray activity and rotation in intermediate-mass G giants
I study the relation between X-ray activity and rotation amongintermediate-mass single G giants. The results show evidence that thequiescent coronal activity of these stars, as measured by their X-raysurface flux, increases linearly with the angular rotation velocity andwith the inverse of the Rossby number. Even the most rapidly rotating Ggiants do not reach the canonical log(L_X/Lbol) ≈ -3saturation level. The effect of rapid rotation on these stars couldresult mainly in an increased coverage of their surface with magneticclose loop structures. The empirical activity-rotation relationshipaccounts for the occurrence of a maximum of magnetic activity in theatmosphere of intermediate-mass stars as they evolve off themain-sequence near the bottom of the red giant branch. Remarkably, therelation between X-ray to bolometric luminosity ratio and the Rossbynumber or rotation period for G giants differs from the power lawdependence with an index of about -2 that is observed for main-sequencestars. Possible implications for the dynamo generation of magneticfields on giants are discussed.
| Rotation and Lithium Surface Abundances, Revisited
For giants in the Hertzsprung gap, the relations betweenTeff, vsini, and lithium surface abundances arereinvestigated and compared with the relations found for Hyadesmain-sequence F stars. For the Hyades main-sequence F stars, the vsinidecrease steeply around Teff~6450 K. At the same temperaturethe lithium surface abundances show a narrow, deep dip. For most giantsthere is also a steep decrease of vsini for Teff around 6450K. At this temperature the lithium surface abundances of the giants alsodecrease steeply and remain low for Teff<6400 K. Thechanges in rotation and Li surface abundances occur over a temperatureinterval of less than 300 K, which for a 2 Msolar giantcorresponds to an age interval of about 106 yr. Thesimultaneous steep decreases of rotation velocities and Li surfaceabundances indicate that for the giants these changes are due to thesame cause, which we suggest to be deep mixing. It then seems ratherlikely that for the Hyades main-sequence F5 V stars the decrease ofrotation and Li surface abundance is also caused by deep mixing. Wesuggest that in both cases the changes are related to the merging of thehydrogen and helium convection zones.
| Rotation Velocities of Red and Blue Field Horizontal-Branch Stars
We present measurements of the projected stellar rotation velocities(vsini) of a sample of 45 candidate field horizontal-branch (HB) starsspanning a wide range of effective temperatures, from red HB stars withTeff~=5000K to blue HB stars with Teff of 17,000K.Among the cooler blue HB stars (Teff=7500-11500 K), weconfirm prior studies showing that, although a majority of stars rotateat vsini<15kms-1, there exists a subset of ``fastrotators'' with vsini as high as 30-35 km s-1. All but one ofthe red HB stars in our sample have vsini<10kms-1, and noanalogous rotation bimodality is evident. We also identify anarrow-lined hot star (Teff~=16,000K) with enhancedphotospheric metal abundances and helium depletion, similar to theabundance patterns found among hot BHB stars in globular clusters, andfour other stars that may also belong in this category. We discussdetails of the spectral line fitting procedure that we use to deducevsini and explore how measurements of field HB star rotation may shedlight on the issue of HB star rotation in globular clusters.
| Observational constraints for lithium depletion before the RGB
Precise Li abundances are determined for 54 giant stars mostly evolvingacross the Hertzsprung gap. We combine these data with rotationalvelocity and with information related to the deepening of the convectivezone of the stars to analyse their link to Li dilution in the referredspectral region. A sudden decline in Li abundance paralleling the onealready established in rotation is quite clear. Following similarresults for other stellar luminosity classes and spectral regions, thereis no linear relation between Li abundance and rotation, in spite of thefact that most of the fast rotators present high Li content. The effectsof convection in driving the Li dilution is also quite clear. Stars withhigh Li content are mostly those with an undeveloped convective zone,whereas stars with a developed convective zone present clear sign of Lidilution.Based on observations collected at ESO, La Silla, Chile, and at theObservatoire de Haute Provence, France, operated by the Centre Nationalde la Recherche Scientifique (CNRS).
| Interrelations between V il and S tr photometric systems: The luminosity indicator (v - X)
Using the largest database of near-IR Ca II Triplet indices currentlyavailable (Cenarro et al. \cite{Cenarro01a},b), we confirm our findingabout the influence of the Ca II stellar lines on the X magnitude ofthe Vilnius photometric system. This effect is significant for spectralsub-classes from early F until mid K. For this spectral range there is alinear relation between the v-X index and the strength of the infraredCa II Triplet, which implies that the Ca II H&K lines shouldinfluence the difference in a similar way. For the spectral intervalstudied, v-X repeats the behavior of the Ca II Triplet with respect togravity, temperature and metallicity. The Ca II Triplet lines are apowerful diagnostic of the stellar populations in galaxies because oftheir sensitivity to the main stellar atmospheric parameters. Being mucheasily achievable observationally and virtually reddening free, the v-Xindex may find similar applications. v-X is log g sensitive butadditional means are required to break the dwarf - giant duplicity. Forthis purpose we have studied the variation of thev(Strömgren)-B(Johnson) index with gravity, temperature and theequivalent width of the Ca II Triplet. Sincev(Strömgren)-B(Johnson) have a none overlapping variation with theCa II Triplet the dwarfs and giants may be separated and Teffand log g may be estimated. The v(Strömgren)-B(Johnson) index hasfurthermore the advantage that E(v-B) ~ 0.25E(B-V).Based on CDS data.
| The Hamburg/RASS Catalogue of optical identifications. Northern high-galactic latitude ROSAT Bright Source Catalogue X-ray sources
We present the Hamburg/RASS Catalogue (HRC) of optical identificationsof X-ray sources at high-galactic latitude. The HRC includes all X-raysources from the ROSAT Bright Source Catalogue (RASS-BSC) with galacticlatitude |b| >=30degr and declination delta >=0degr . In thispart of the sky covering ~ 10 000 deg2 the RASS-BSC contains5341 X-ray sources. For the optical identification we used blue Schmidtprism and direct plates taken for the northern hemisphere Hamburg QuasarSurvey (HQS) which are now available in digitized form. The limitingmagnitudes are 18.5 and 20, respectively. For 82% of the selectedRASS-BSC an identification could be given. For the rest either nocounterpart was visible in the error circle or a plausibleidentification was not possible. With ~ 42% AGN represent the largestgroup of X-ray emitters, ~ 31% have a stellar counterpart, whereasgalaxies and cluster of galaxies comprise only ~ 4% and ~ 5%,respectively. In ~ 3% of the RASS-BSC sources no object was visible onour blue direct plates within 40\arcsec around the X-ray sourceposition. The catalogue is used as a source for the selection of(nearly) complete samples of the various classes of X-ray emitters.
| The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. II. Basic Parameters of Program Stars and the Role of Microturbulence
Paper I of this series presented precise MK spectral types for 372 lateA-, F-, and early G-type stars with the aim of understanding the natureof luminosity classification on the MK spectral classification systemfor this range of spectral types. In this paper, a multidimensionaldownhill simplex technique is introduced to determine the basicparameters of the program stars from fits of synthetic spectra andfluxes with observed spectra and fluxes from Strömgren uvbyphotometry. This exercise yields useful calibrations of the MK spectralclassification system but, most importantly, gives insight into thephysical nature of luminosity classification on the MK spectralclassification system. In particular, we find that in this range ofspectral types, microturbulence appears to be at least as important asgravity in determining the MK luminosity type.
| The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars
This is the first in a series of two papers that address the problem ofthe physical nature of luminosity classification in the late A-, F-, andearly G-type stars. In this paper, we present precise spectralclassifications of 372 stars on the MK system. For those stars in theset with Strömgren uvbyβ photometry, we derive reddenings andpresent a calibration of MK temperature types in terms of the intrinsicStrömgren (b-y)0 index. We also examine the relationshipbetween the luminosity class and the Strömgren c1 index,which measures the Balmer jump. The second paper will address thederivation of the physical parameters of these stars, and therelationships between these physical parameters and the luminosityclass. Stars classified in this paper include one new λ Bootisstar and 10 of the F- and G-type dwarfs with recently discoveredplanets.
| CaII K Emission-Line Asymmetry among Red Giants Detected by the ROSAT Satellite
Spectra of the Ca II H and K lines are reported for a number of fieldgiants from which soft X-ray emission was detected by the ROSATsatellite. Several of these stars are RS CVn systems and exhibit verystrong Ca II emission. The majority of the noninteracting giants in thesample have MV>-2.0, as determined from Hipparcosparallaxes, and spectral types earlier than K3. The Ca II Kemission-line profile for these stars is most often double-peaked andasymmetric, with the short-wavelength peak being stronger than thelongward peak. This asymmetry is in the same sense as for the integrateddisk of the Sun. The X-ray and Ca II K-line data indicate that giants ofspectral types G and early K have coronae and chromospheres seeminglyanalogous to those of the Sun. Four M giants that were detected by ROSATwere also observed. Their Ca II emission spectra show asymmetries inwhich the violet wing is weaker than the red wing, a phenomenon that istypical of M giants in general and indicative of mass outflows in theirchromospheres. The majority of these M giants, but not all, are known tobe in binary systems, so it is possible that the X-ray emission for atleast some of them may come from a companion. Alternatively, some or allof these M giants may be examples of hybrid stars.
| Rotation and lithium in single giant stars
In the present work, we study the link between rotation and lithiumabundance in giant stars of luminosity class III, on the basis of alarge sample of 309 single stars of spectral type F, G and K. We havefound a trend for a link between the discontinuity in rotation at thespectral type G0III and the behavior of lithium abundances around thesame spectral type. The present work also shows that giant starspresenting the highest lithium contents, typically stars earlier thanG0III, are those with the highest rotation rates, pointing for adependence of lithium content on rotation, as observed for otherluminosity classes. Giant stars later than G0III present, as a rule, thelowest rotation rates and lithium contents. A large spread of about fivemagnitudes in lithium abundance is observed for the slow rotators.Finally, single giant stars with masses 1.5 < M/Msun<=2.5 show a clearest trend for a correlation between rotational velocityand lithium abundance. Based on observations collected at theObservatoire de Haute -- Provence (France) and at the European SouthernObservatory, La Silla (Chile). Table 2 is only available electronicallywith the On-Line publication athttp://link.springer.de/link/service/00230/
| 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
| Evolution of X-ray activity and rotation on G-K giants
The recent availability of stellar parallaxes provided by the Hipparcosstar catalogue (ESA 1997) enables an accurate determination of thepositions of single field giants in a theoretical H-R diagram and areliable estimate of their masses. The present study combines these newastrometric data with previously published X-ray fluxes and rotationalvelocities. The results confirm the existence of a sharp decrease ofX-ray emission at spectral type K1 for 2.5 M_sun < M < 5 M_sungiants. The study shows that the rotational velocity of these starsreaches a minimum at the same location in the H-R diagram. However, notight relationship between X-ray luminosities and projected equatorialvelocities was found among the sample stars. I suggest that theseresults could reflect the importance of differential rotation indetermining the level of coronal emission among >= 2.5Msun G and K giants. The restoration of rigid rotation at thebottom of the red giant branch could prevent the maintenance of largescale magnetic fields, thus explaining the sharp decrease of coronalX-ray emission at spectral type K1.
| The Coronae of Moderate-Mass Giants in the Hertzsprung Gap and the Clump
We have used the Roentgensatellit (ROSAT), the Extreme UltravioletExplorer (EUVE), and the Hubble Space Telescope (HST) to measure X-rayand ultraviolet emissions of moderate-mass (~2-3 Mȯ) giants in theHertzsprung gap (spectral types early F to mid-G) and the post-heliumflash "clump" (~G8-K0). Our motivation was to document the evolution ofhot coronae (T > 106 K) along the post-main-sequence trajectoriestraveled by such stars in order to gain insight concerning the "X-raydeficiency" of the F-G0 giants and the strong braking of stellarrotation at the red edge of the Hertzsprung gap. With few exceptions,Hertzsprung gap and clump giants observed by ROSAT PSPC show hot (T ~107 K) coronal energy distributions, regardless of any X-ray deficiency.EUVE spectra of gap star 31 Com (G0 III) indicate a broad coronalemission measure hump at ~107.2 K, while the active clump giant betaCeti (K0 III) displays a sharp peak at ~106.8 K, as seen previously inthe mixed clump/gap binary Capella ( alpha Aur: G8 III + G0 III). Thegap giants upsilon Peg (F8 III) and 24 UMa (G4 III) have EUV emissionsof intermediate temperature (~107.0 K). The stars 31 Com, psi 3 Psc (G0III), and beta Cet exhibit redshifted transition zone (TZ: ~105 K) linesin HST GHRS spectra, as reported earlier in Procyon ( alpha CMi: F5IV-V) and Capella G0. Such redshifts on the Sun are thought to signifyflows in magnetic loops. beta Cas (F2 III)--a rare soft coronal sourceamong the gap stars--displays blueshifts of C IV and O IV], althoughemissions at cooler and hotter temperatures are near the photosphericvelocity. The remarkably broad line profiles of the fastest rotating gapgiants suggest that the 105 K "subcoronal" emission zones extend to h~R_{*} above the photosphere, about 50 scale heights. In contrast to theTZ line redshifts, the upper chromospheric emissions (e.g., Mg II and SiIII) of 31 Com and psi 3 Psc have blueshifted cores. Blue-asymmetricpeaks in the solar Mg II lines are thought to indicate dynamical heatingin the chromosphere. Observations of the H I Ly alpha feature of 31 Comtaken 9 months apart reveal striking profile changes, reminiscent ofthose noted previously in the Ly alpha blue peak of the Capella G0 star.We used the far-ultraviolet diagnostics, in combination with ROSAT X-rayphotometry and EUVE high-excitation line strengths, to constrainphysical models of the stellar outer atmospheres. Quasi-static magneticloops can simulate the empirical coronal emission measures of the giantstars, but the inferred pressures for sensible loop lengths conflictwith direct measurements of subcoronal densities. Furthermore, the highrate of emission at ~105 K cannot be explained by thermal conductiondown the legs of hot quasi-static loops. On the other hand, the possibleexistence of elongated (l ~ R_{*} ) emission structures on the gapgiants leads to a speculative scenario to explain the X-ray deficiency.It is based on the increased importance of the dynamical filling phase("explosive evaporation") of the loop life cycle; conductive cooling,yielding TZ emissions at the footpoints, when the heating isinterrupted; and the possibility for transitions between "hot" and"cool" energy balance solutions owing to dynamical suspension andcentrifugal trapping of the cooling gas. The long loops might representa vestigial global "magnetosphere" inherited from the main-sequencephase, which ultimately is disrupted near ~G0 by the deepeningconvective envelope and growth of a more solar-like dynamo. Coronalemissions might be boosted temporarily as the X-ray deficiency isremoved but soon would be quenched by wind braking previously inhibitedby the magnetospheric "dead zone."
| The ROSAT all-sky survey catalogue of optically bright late-type giants and supergiants
We present X-ray data for all late-type (A, F, G, K, M) giants andsupergiants (luminosity classes I to III-IV) listed in the Bright StarCatalogue that have been detected in the ROSAT all-sky survey.Altogether, our catalogue contains 450 entries of X-ray emitting evolvedlate-type stars, which corresponds to an average detection rate of about11.7 percent. The selection of the sample stars, the data analysis, thecriteria for an accepted match between star and X-ray source, and thedetermination of X-ray fluxes are described. Catalogue only available atCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| High Chromospheres of Late A Stars
We report the detection of N V 1239 A transition region emission inHST/Goddard High Resolution Spectrograph spectra of the A7 V stars,alpha Aql and alpha Cep. Our observations provide the first directevidence of 1--3 x 105 K material in the atmospheres of normal A-typestars. For both stars, and for the mid A-type star tau 3 Eri, we alsoreport the detection of chromospheric emission in the Si III 1206 Aline. At a B-V color of 0.16 and an effective temperature of ~8200 K,tau 3 Eri becomes the hottest main-sequence star known to have achromosphere and, thus, an outer convection zone. We see no firmevidence that the Si III line surface fluxes of the A stars are anylower than those of moderately active, solar-type G and K stars. Thiscontrasts sharply with their coronal X-ray emission, which is more than100 times weaker than that of the later type stars. Given the strengthof the N V emission observed here, it now appears unlikely that theX-ray faintness of A stars is due to their forming very cool, <=1 MKcoronae. An alternative explanation in terms of mass loss in coronalwinds remains a possibility, though we conclude from moderate resolutionspectra of the Si III lines that such winds, if they exist, do notpenetrate into the chromospheric Si III--forming layers of the star,since the profiles of these lines are not blueshifted and may well beredshifted with respect to the star.
| An Atlas of the infrared spectral region. II. The late-type stars (G - M)
This Atlas illustrates the behavior of late type stars (F, G, K and M)in the near infrared 8400-8800 Angstrom region with a resolution ofabout 2 degrees. Seventeen figures illustrate the spectral sequence andluminosity classes V, III, Ib and Ia. Four figures illustrate peculiarspectra, namely those of Am stars, composites, weak metal stars and Sand C type objects. The complete Atlas is also available as FITS filesfrom the CDS de Strasbourg and other data centers.
| A spectroscopic search for high azimuthal-order pulsation in broad-lined late F- and early G-stars.
During 3 consecutive nights, 13 southern F- and G-type dwarfs and giantsoutside the conventional δ Scuti instability strip were observedat high spectral (3km/s) and medium temporal (10-15min) resolution. Thestars were selected for their reported broad spectral lines(vsini>=40km/s) so that pulsation in higher azimuthal-order nonradialharmonics could, via the rotational Doppler effect, reveal itself byline profile variability. Two stars turned out to have very narrowlines, one was confirmed as a short-period double-lined binary. Lineprofile ondulations typical of pulsation with azimuthal order8<=m<=14 were detected in δ Aql and ɛ2Ara. In addition, ɛ2 Ara displayed line profiledistortions at a larger scale as they would result from a mode with m~4.The observational sampling of all three variabilities constrainspossible periods only poorly. However, if the variations are periodic,they may well be too slow for p-mode oscillations. This would suggest arelation to the new class of γ Dor variables in which g-modes seemto be excited. If so, the two stars could be the first γ Dor starswith detected higher nonradial-harmonic pulsation. While uvby photometryplaces δ Aql still just within the δ Scuti strip,ɛ2 Ara would be the reddest candidate γ Dorstar to date. For the remaining 8 stars, upper amplitude limits between2 and 6km/s were derived for nonradial mode orders 6<=m<=16 andp-modes with periods ~20minutes. In 3 stars narrow absorption lines weredetected which probably are due to a cool companion.
| On the Determination of Empirical Stellar Flux Scales
Several studies have appeared in the literature describing methods forderiving stellar continuum fluxes as simple functions of Johnson colorindices. In previous papers, we have used similar relations to derive CaII H and K line core fluxes for dwarf stars on Lowell Observatory'sSolar-Stellar Spectrograph (SSS) program. Our desire is to present ourdata, and complementary data from the Mt. Wilson and National SolarObservatory stellar and solar programs, in terms of physical fluxes.However, our existing relations break down for mid-K and later stars andfor giant stars, which form an important element of our target list. Inthis work I have used a broader range of spectrophotometry and angulardiamters than in our previous work to derive empirical flux scales forspectral types A to early M, luminosity classes I to V, and for fourcolor indices, Johnson B-V, V-R, R-I, and Stromgren b-y. In this paper,I describe the methods I used and present the desired flux scales. Icompare the results with those from earlier studies and present examplesof the use of the flux scales. The data and results are available on theWorld Wide Web. (SECTION: Stars)
| A Search for Optical Flares in Chromospherically Active Stars
We have surveyed four years of archival UBV photometry of 69chromospherically active stars obtained with the Phoenix-10 automaticphotoelectric telescope in search of optical flares on these stars. Wedemonstrate taht, while flares can be detected in these data, the numberof events observed on evolved stars remains very small. Flares werefound only on UX Arietis, II Pegasi, and AR Piscium. (SECTION: Stars)
| Classification of Population II Stars in the Vilnius Photometric System. I. Methods
The methods used for classification of Population II stars in theVilnius photometric system are described. An extensive set of standardswith known astrophysical parameters compiled from the literature sourcesis given. These standard stars are classified in the Vilnius photometricsystem using the methods described. The accuracy of classification isevaluated by a comparison of the astrophysical parameters derived fromthe Vilnius photometric system with those estimated from spectroscopicstudies as well as from photometric data in other systems. For dwarfsand subdwarfs, we find a satisfactory agreement between our reddeningsand those estimated in the uvbyscriptstyle beta system. The standarddeviation of [Fe/H] deter mined in the Vilnius system is about 0.2 dex.The absolute magnitude for dwarfs and subdwarfs is estimated with anaccuracy of scriptstyle <=0.5 mag.
| 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.
| The RIASS coronathon: Joint X-ray and ultraviolet observations of normal F-K stars
Between 1990 August and 1991 January the ROSAT/IUE All Sky Survey(RIASS) coordinated pointings by the International Ultraviolet Explorer(IUE) with the continuous X-ray/EUV mapping by the Roentgensatellit(ROSAT). The campaign provided an unprecedented multiwavelength view ofa wide variety of cosmic sources. We report findings for F-K stars, alarge proportion of the RIASS targets. Forty-eight of our 91'Coronathon' candidates were observed by the IUE during the campaign.For stars missed by the IUE, we supplemented the ROSAT survey fluxeswith archival UV spectra and/or follow-on observations.
| A Study of the Chromospherically Active, Short-Period Binary VZ PISCIUM
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJ...455..300H&db_key=AST
| H-alpha measurements for cool giants
The H-alpha line in a cool star is usually an indication of theconditions in its chromosphere. I have collected H-alpha spectra of manynorthern G-M stars, which show how the strength and shape of the H-alphaline change with spectral type. These observations detect surprisinglittle variation in absoption-line depth (Rc approximately0.23 +/- 0.08), linewidth (FWHD approximately 1.44 +/- 0.22 A), orequivalent width (EW approximately 1.12 +/- 0.17 A) among G5-M5 IIIgiants. Lines in the more luminous stars tend to be broader and strongerby 30%-40% than in the Class III giants, while the H-alpha absorptiontends to weaken among the cooler M giants. Velocities of H-alpha andnearby photospheric lines are the same to within 1.4 +/- 4.4 km/s forthe whole group. To interpret these observations, I have calculatedH-alpha profiles, Ly-alpha strengths, and (C II) strengths for a seriesof model chromospheres representing a cool giant star like alpha Tau.Results are sensitive to the mass of the chromosphere, to chromospherictemperature, to clumping of the gas, and to the assumed physics of lineformation. The ubiquitous nature of H-alpha in cool giants and the greatdepth of observed lines argue that chromospheres of giants cover theirstellar disks uniformly and are homogeneous on a large scale. This isquite different from conditions on a small scale: To obtain a highenough electron density with the theoretical models, both to explain theexitation of hydrogen and possibly also to give the observed C IImultiplet ratios, the gas is probably clumped. The 6540-6580 A spectraof 240 stars are plotted in an Appendix, which identifies the date ofobservation and marks positions of strong telluric lines on eachspectrum. I assess the effects of telluric lines and estimates that thestrength of scattered light is approximately 5% of the continuum inthese spectra. I give the measurements of H-alpha as well as equivalentwidths of two prominent photospheric lines, Fe I lambda 6546 and Ca Ilambda 6572, which strengthen with advancing spectral type.
| 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.
| An atlas of the infrared spectral region. I. The early type stars (O-G0).
The Atlas illustrates the behavior of early type stars (O, B, A and Ftype) in the near infrared 8375-8770A region at a resolution of aboutone A. Intensity tracings of 76 stars are presented. Of these 51 starscover the spectral range O to G0 and luminosity classes V, III, Ib andIa. The influence of the rotational velocity is also illustrated as wellas the spectra of 19 stars with spectral peculiarities. The completeAtlas is also available under catalog number 3183 from the CDSStrasbourg and other data centers.
| On the link between rotation and coronal activity in evolved stars.
We analyse the behaviour of coronal activity as a function of rotationfor a large sample of single and binary evolved stars for which we haveobtained CORAVEL high precision rotational velocities. This study showsthat tidal effects play a direct role in determining the X-ray activitylevel in binary evolved stars. The circularisation of the orbit is anecessary property for enhanced coronal activity in evolved binarystars.
| The active dynamo stars: RS CVn, BY Dra, FK Com, Algol, W UMa, and T Tau
Not Available
| The lithium content and other properties of F2-G5 giants in the Hertzsprung Gap
As stars of 2-5 solar mass evolve across the Hertzsprung Gap they shouldfirst deplete their surface lithium by convective dilution and then,when convection penetrates deeper, begin to bring CN processed materialto their surfaces. To investigate this process we have observed 52giants, 25 of which have known C/N ratios, for their Li abundances.After eliminating four stars that may actually be dwarfs and includingthe two components of Capella analyzed by Pilachowski and Sowell we havecompared our (Li/Fe) ratios with models of Swenson. For stars showing vsin i greater than 50 km/s we find (Li/Fe) to be unaffected by mixingfor B - V less than 0.7 as predicted. For stars cooler than B - V = 0.7both v sin i and (Li/Fe) drop to smaller values. For the sharp linedstars (v sin i less than 50 km/s) we find a drop in Li between B - V =0.45 and 0.60 which cannot be understood in terms of dilution byconvection. Various possible causes of such an early depletion ordilution of surface Li are discussed including diffusion at the base ofthe convection zone, mass loss possibly enhanced by pulsation, andmagnetic activity as in the magnetic A and B type stars. The models ofRicher & Michaud (1993) with diffusion point toward a satisfactorysolution. A few giants with low v sin i values stand out with muchhigher than expected (Li/Fe) values despite their cool effectivetemperatures. We do not understand why those stars have not depletedtheir lithium as have most giants of similar color. The correlation of(N/C) with (Li/Fe) follows expectations in so far as almost all starswith enhanced (N/C) have depleted their Li as well.
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