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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.
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sonraki gruplarýn üyesi:
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Calgi |
| Sað Açýklýk: | 19h05m12.27s |
| Yükselim: | +31°26'21.1" |
| Görünürdeki Parlaklýk: | 7.723 |
| Uzaklýk: | 558.659 parsek |
| özdevim Sað Açýklýk: | -1.4 |
| özdevim Yükselim: | -2.8 |
| B-T magnitude: | 9.009 |
| V-T magnitude: | 7.83 |
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