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Long-term monitoring of active stars. IX. Photometry collected in 1993
As a part of an extensive program focused on the global properties andevolution of active stars, high-precision UBV(RI)_c and UBV photometryof 31 selected stars is presented. The UBV(RI)_c observations werecollected at the European Southern Observatory over the 31 December1992-18 January 1993 and the 20 November-3 December 1993 intervals.Additional UBV photometry obtained by the ``Phoenix" and by the CataniaAstrophysical Observatory Automatic Photoelectric Telescopes from 1990to 1993 is also presented for some of the program stars. Significantevolution of the light curves, period variations and evidence forlong-term variability of the global degree of spottedness are found.Some spectral classifications are revised and the inferred photometricparallaxes are compared, whenever possible, with the values measured bythe Hipparcos satellite. These observations are finalized to theconstruction of an extended photometric database, which can giveimportant clues on topics such as the stability of spotted areas,differential rotation, solar-like cycles and the correlation betweeninhomogeneities at different atmospheric levels. Based on data collectedat the European Southern Observatory, La Silla, Chile. Tables and thecomplete data set are also available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/910
| UBVRI photometry of FKSZ stars. IV
The paper presents UBVRI photometry, in the Kron-Cousins system, for 117stars of the Catalog of Fundamental Faint Stars in the declination zone+18-0 deg. The observations were performed from July 1988 to March 1990with the ESO 0.50-m telescope at the ESO in La Silla, Chile. The resultsof 24 nights of observations are reported.
| Photometric variability in chromospherically active stars. III - The binary stars
Differential UBV photometry of 49 late-type chromospherically activebinary stars has been obtained. A total of 12,353 differential UBVmagnitudes have been acquired and are used to determine seasonalphotometric periods, amplitudes, mean brightnesses, maximum spotamplitudes, 'unspotted' differential magnitudes, and times of minimumlight. Standard Fourier techniques are used to investigate the cause ofthe light variability. Eight stars are found which exhibit lightvariations due not to spot activity but rather to ellipticity and/orreflection effect. Others show combinations of all three effects. Someof the systems also show substantial differences between theirrotational and orbital period.
| Light and colour curve observations and analysis of the short period eclipsing binary system UV PSC
In the present work B and V light curves and the (B-V)-color curve ofthe short period (RS CVn type) binary system UV Psc are presented andanalyzed, and absolute information from the available data are derived.Chi-squared minimization procedures were utilized to a large extent infitting light and color curves. The solutions show the binary to be at adistance of about 90 pc with two detached components which are close tothe main sequence (G2 and K0). The inclination of the orbit is close to90 deg. Photometric irregularities present in the light curve arebriefly considered in relation to current ideas on RS CVn systems, andthe color information indicates that a locally hotter (rather thancooler) region is responsible for the irregularities.
| UV Psc - a Short Period RS CVn Star
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| Takýmyýldýz: | Baliklar |
| Sað Açýklýk: | 01h18m57.43s |
| Yükselim: | +07°25'49.5" |
| Görünürdeki Parlaklýk: | 8.007 |
| Uzaklýk: | 344.828 parsek |
| özdevim Sað Açýklýk: | -11.6 |
| özdevim Yükselim: | 1 |
| B-T magnitude: | 9.408 |
| V-T magnitude: | 8.123 |
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