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Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| 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 photoelectric investigation of light variability in AP stars
A study of the light variability of a number of peculiar A stars, mainlyin Stromgren colors u and v and in peculiarity index Delta-a, leads tothe proposal of the following light variability periods: (1) HD 5601,1.11 days; (2) HD 19712, 2.19 days; (3) HD 30849, 15.86 days; (4) HD38823, 8.64 days; (5) HD 53116, 11.98 or 18.10 days; (6) HD 56022, 0.92days; and (7) HD 81009, 33.97 days. In addition, evidence is given forvariability of HD 94660 on a time scale on the order of months or years,and it is shown that the rotation period proposed by Borra andLandstreet (1980) for HD 25267 is not supported by the light variationsobserved. The character of Delta-a variability is discussed.
| UVBY and H beta photometry of early-type stars in a region at high galactic latitude.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973AJ.....78...47D&db_key=AST
| The Kreinin-Murri Method for Absolute Determination of Equatorial-Star Declinations.
Not Available
| UBV photometry of early-type stars in two regions at high galactic latitudes
Not Available
| A Finding List of Stars of Spectral Type A7 and Earlier in Regions at High Galactic Latitudes. III. 4 HLF 4
An objective prism survey has been made of stars of spectral type A7 andearlier in a 45 square degree region in the 4 HLF 4 area (l^II =180°, b^II = -45°) as part of an investigation of galacticstructure perpendicular to the galactic plane. The survey reported herewas made with the 4° prism on the Michigan Curtis Schmidt telescopeat Cerro Tololo. A finding list containing positions and spectral typesfor 88 stars is presented with finding charts for the stars too faint tobe included in the Bonner Durchmusterung.
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| Takýmyýldýz: | Balina |
| Sað Açýklýk: | 03h10m35.94s |
| Yükselim: | +00°12'45.0" |
| Görünürdeki Parlaklýk: | 7.282 |
| Uzaklýk: | 127.389 parsek |
| özdevim Sað Açýklýk: | -12.3 |
| özdevim Yükselim: | -34.8 |
| B-T magnitude: | 7.594 |
| V-T magnitude: | 7.308 |
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