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Chromospherically Active Stars. XIX. A Reexamination of the Variability of HD 10909=UV Fornacis
We have obtained new spectroscopy and photometry of the K0 IV,chromospherically active, single-lined spectroscopic binary HD 10909.Those observations show that the previously reported orbital and lightvariability periods are incorrect. HD 10909 has an orbital period of30.1067 days and an eccentricity of 0.499. Its rotation period of 64.1days is more than twice as long as its orbital period. The primary issituated near the base of the first-ascent red giant branch. Thus, itsasynchronous rotation is likely the result of its recent evolutionthrough the Hertzsprung gap, combined with its relatively long orbitalperiod and high eccentricity.
| Photometry of 50 suspected variable stars
Fifty stars have been chosen as suspected variable stars and analyzedfor variability. A large portion of this sample are stars that areeither proved active chromosphere stars or are candidates for suchactivity. The photometric data base consists of differential Vmeasurements of the Vanderbilt 16 inch (41 cm) automatic photoelectrictelescope and 25 observers at 26 observatories worldwide. Publishedphotometric data have also been utilized, with proper adjustments madeto ensure that all magnitudes are differential. Searches for photometricperiod, amplitudes, and times of minimum light showed 68 percent of thesample to be photometrically variable with periods found for 34. Twostars were deemed norvariable for the period of observation. Conclusivestatements could not be made concerning the photometric variability ofthe 14 remaining stars.
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Balina |
| Sað Açýklýk: | 01h44m05.89s |
| Yükselim: | -23°36'02.7" |
| Görünürdeki Parlaklýk: | 9.375 |
| özdevim Sað Açýklýk: | 22.4 |
| özdevim Yükselim: | -6.6 |
| B-T magnitude: | 10.716 |
| V-T magnitude: | 9.486 |
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