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Optical variability of SAO 91772: A serendipitous X-ray source
During the course of systematic observations of known or suspectedchromospherically active stars carried out at Catania AstrophysicalObservatory by a 0.8-m Automated Photometric Telescope (APT), thevariability of SAO 91772, the optical counterpart of the serendipitousX-ray source 1E0009.0+1417, was discovered. We detected aquasi-sinusoidal variation with a period of 1.84 +/- 0.02 days and aV-band peak-to-peak amplitude of about 0.08 magnitudes. The variation ofthe color indices suggests that the light change is due to photosphericcool spots, whose visibility on the projected stellar disk facing theobserver is modulated by the star rotation. Moreover, long-termvariability of the global spot covering factor is strongly suspected.
| Evolved GK stars near the sun. I - The old disk population
A sample of nearly two thousand GK giants with intermediate band, (R,I),DDO and Geneva photometry has been assembled. Astrometric data is alsoavailable for most of the stars. The some 800 members of the old diskpopulation in the sample yield accurate luminosities (from two sources),reddening values and chemical abundances from calibrations of thephotometric parameters. Less than one percent of the objects arepeculiar in the sense that the flux distribution is abnormal. Thepeculiarity is signaled by strong CH (and Ba II) and weak CH. The CH+stars are all spectroscopic binaries, probably with white dwarfcompanions, whereas the CH- stars are not. A broad absorption band,centered near 3500 A, is found in the CH+ stars whereas the CH- objectshave a broad emission feature in the same region. The intensity of theseabsorptions and emissions are independent of the intensity of abnormalspectral features. Ten percent of the old disk sample have a heavyelement abundance from one and a half to three times the solar value.The distribution of the heavy element abundances is nearly a normal onewith a peak near solar abundance and ranges three times to one sixthsolar. The distribution of the (U, V) velocities is independent of theheavy element abundance and does not appear to be random. Ten percent ofthe old disk stars show a CN anomaly, equally divided between CN strongand CN weak. Several stars of individual astrometric or astrophysicalimportance are isolated.
| Large and kinematically unbiased samples of G- and K-type stars. V - Evolved stars in the selected areas at + 15-deg declination
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1990PASP..102..242E&db_key=AST
| Photoelectric radial velocities. IV. 528 7 to 10 mag stars in the +15degree selected areas.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971MNRAS.155....1G&db_key=AST
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Miembro de los siguientes grupos:
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Datos observacionales y astrométricos
| Constelación: | Piscis, Peces |
| Ascensión Recta: | 00h16m02.05s |
| Declinación: | +14°42'26.3" |
| Magnitud Aparente: | 8.382 |
| Distancia: | 197.239 parsecs |
| Movimiento Propio en Ascensión Recta: | 68.6 |
| Movimiento Propio en Declinación: | -15.7 |
| B-T magnitude: | 10.115 |
| V-T magnitude: | 8.526 |
Catálogos y designaciones:
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