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Mixing along the red giant branch in metal-poor field stars
We have determined Li, C, N, O, Na, and Fe abundances, and12C/13C isotopic ratios for a sample of 62 fieldmetal-poor stars in the metallicity range -2<=[Fe/H]<= -1. Starswere selected in order to have accurate luminosity estimates from theliterature, so that evolutionary phases could be clearly determined foreach star. We further enlarged this dataset by adding 43 more starshaving accurate abundances for some of these elements and similarly welldefined luminosities from the literature. This large sample was used toshow that (small mass) lower-RGB stars (i.e. stars brighter than thefirst dredge-up luminosity and fainter than that of the RGB bump) haveabundances of light elements in agreement with predictions fromclassical evolutionary models: only marginal changes occur for CNOelements, while dilution within the convective envelope causes thesurface Li abundance to decrease by a factor of ~ 20. A second, distinctmixing episode occurs in most (perhaps all) small mass metal-poor starsjust after the RGB bump, when the molecular weight barrier left by themaximum inward penetration of the convective shell is canceled by theoutward expansion of the H-burning shell, in agreement with recenttheoretical predictions. In field stars, this second mixing episode onlyreaches regions of incomplete CNO burning: it causes a depletion of thesurface 12C abundance by about a factor of 2.5, and acorresponding increase in the N abundance by about a factor of 4. The12C/13C is lowered to about 6 to 10 (close to butdistinctly higher than the equilibrium value of 3.5), while practicallyall remaining Li is burnt. However an O-Na anti-correlation such astypically observed amongst globular cluster stars, is not present infield stars. None of the 29 field stars more evolved than the RGB bump(including 8 RHB stars) shows any sign of an O depletion or Naenhancement. This means that the second mixing episode is not deepenough to reach regions were ON-burning occurs in field stars. Based inpart on observations made at the ESO La Silla ObservatoryTables 1, 2, 3, 5 and 6 are available in electronic form only at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Ca II H and K Photometry on the UVBY System. III. The Metallicity Calibration for the Red Giants
New photometry on the uvby Ca system is presented for over 300 stars.When combined with previous data, the sample is used to calibrate themetallicity dependence of the hk index for cooler, evolved stars. Themetallicity scale is based upon the standardized merger of spectroscopicabundances from 38 studies since 1983, providing an overlap of 122evolved stars with the photometric catalog. The hk index producesreliable abundances for stars in the [Fe/H] range from -0.8 to -3.4,losing sensitivity among cooler stars due to saturation effects athigher [Fe/H], as expected.
| SANTIAGO 91, a right ascension catalogue of 3387 stars (equinox J2000).
The positions in right ascension of 3387 stars belonging to the Santiago67 Catalogue, observed with the Repsold Meridian Circle at Cerro Calan,National Astronomical Observatory, during the period 1989 to 1994, aregiven. The average mean square error of a position, for the wholeCatalogue, is +/-0.009 s. The mean epoch of the catalogue is 1991.84.
| Reddening estimation for halo red giants using UVBY photometry
Updated uvby observations for a larger sample of metal-deficient redgiants are presented and combined with a select sample of data from theliterature transformed to a common system. Using the reddening maps ofBurstein & Heiles (1982), new absolute magnitudes, distances,metallicities, and reddenings are derived for each star. Themetallicities are determined with a revised calibration of them1, (b-y) diagram based upon comparison to a complilation ofrecent spectrsoscopic abundances transformed to a common system. Thephotometric abundances agree very well with the spectroscopic; thedispersion among the residuals for 58 giants is +/- 0.16 dex. Thedereddened indices are used to show that for red giants with (Fe/H) lessthan -1.5, there is a well-defined relation in the c0,(b-y)0 diagram which exhibits only a weak dependence uponmetallicity. Use of the standard relations allows one to obtainreddening estimates for normal halo field giants and globular clustersin the appropriate metallicity range.
| Astrometric and astrophysical discontinuities between the galactic old disk and halo stellar populations
Intermediate band, RI, and DDO photometry of the weak-lined stars in thefirst three volumes of the Michigan catalogs of spectral type arediscussed on the basis of luminosity and heavy element abundance. Theinterface between the old disk (Fe/H greater than -0.8 dex) and halo(Fe/H less than -1.2 dex) populations represents discontinuities in boththe stellar motions and the stellar physics. The CN strengths of bothevolved and unevolved halo stars decrease with decreasing temperature,in a mirror image of the increase with decreasing temperature for thedisk objects. The result for the halo giants has been attributed to deepmixing in the stellar atmospheres but the similar result for unevolveddwarfs indicates a difference in formation rather than in evolutionaryprocess of the two populations.
| Walraven photometry of nearby southern OB associations
Homogeneous Walraven (VBLUW) photometry is presented for 5260 stars inthe regions of five nearby southern OB associations: Scorpio Centaurus(Sco OB2), Orion OB1, Canis Major OB1, Monoceros OB1, and Scutum OB2.Derived V and (B - V) in the Johnson system are included.
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Observation and Astrometry data
| Constellation: | Σκορπιός |
| Right ascension: | 16h49m08.12s |
| Declination: | -27°34'14.8" |
| Apparent magnitude: | 8.914 |
| Distance: | 12500 parsecs |
| Proper motion RA: | -8 |
| Proper motion Dec: | 24.9 |
| B-T magnitude: | 9.962 |
| V-T magnitude: | 9.001 |
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