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UBV absolute CCD photometry and differential astrometry of a sample of visual double stars with A-type primaries
We present V magnitudes, (B-V) and (U-B) colours of the components of111 visual double stars and their relative position measurements rho andtheta . The primaries are of spectral class A; the angular separation isin the 2farcs5 -8arcsec range. The observations were made at the 61-cmreflector of University of Toronto Southern Observatory, Chile. Theobtained photometric results are of a moderate quality for absolutevalues (0.04() m (mag) in V and about 0.02() m in the (B-V) and (U-B)colour indices) and more precise in Delta V and Delta (U-B), Delta (B-V)(0.023() m and 0.015() m, respectively). We find that about 60% ofsecondaries are also of spectral type A; 56% of pairs have Delta (B-V)less than 0.1() m. The two-colour diagram reveals significant offset ofobjects from the curve of unreddened Main Sequence stars. Acomprehensive survey of stars in the close vicinity to the objects isalso presented. The final astrometric accuracy of ~ 0farcs01 in rho and0fdg1 in theta provides additional measurements for study of relativemotion of the components. Based on observations made at University ofToronto Southern Observatory, Las Campanas, Chile. Tables\arabic{tabptm}--\arabic{tabast} are only available in electronic format the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) orvia http://cdsweb.u-strasbg.fr/Abstract.html
| The MK classification and its calibration
The system of spectral classification is described as it has developedfrom the original Yerkes Atlas (Morgan, Keenan, Kelman 1943) untiltoday. The word 'developed' is used because any system that is to remainuseful must be flexible enough to adapt not only to improved techniquesof measurement but also to new theoretical insights into the variablesthat actually determine the energy spectrum of a star in all itsfascinating but sometimes frustrating detail. The discussion does notconsider the criteria of classification but is confined to the resultingset of temperature types and luminosity classes. Chemical composition isexamined as a third variable. Tabulated and plotted informationincludes: MK temperature subclasses; lists of MK types of fainter stars;published calibrations of luminosity classes for early-type stars;calibration of MK luminosity classes for types later than F8; thedistribution among groups of the 426 stars in the author's current listof best types; and the effects of metal deficiencies on spectra of KOIII stars. The revised MK classification can be applied to all but a fewpercent of the stars later in type than GO. For the two-thirds of thesethat have approximately solar composition no abundance index is needed;for most of the remainder one abundance index suffices.
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Посматрања и Астрометриски подаци
| Сазвежђа: | Прамац |
| Ректацензија: | 10h28m49.90s |
| Deклинација: | -66°41'47.5" |
| Apparent магнитуда: | 9.223 |
| Даљина: | 763.359 parsecs |
| Proper motion RA: | -32.3 |
| Proper motion Dec: | 32.5 |
| B-T magnitude: | 9.304 |
| V-T magnitude: | 9.23 |
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