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The MAIA candidate star HD 208727
HD 208727 is a suspected member of the enigmatic MAIA variables andshows the largest yet observed amplitude in light variation for any ofthe potential members. Proven beyond doubt pulsation would pose aserious problem for stellar modelling and opacities, because eitheropacity source for driving pulsation has to be a different or newidentified, yet unkown, pulsation mechanism. We conclude from ourinvestigation that rotation is a more likely explanation for the lightvariability of HD 208727.
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| Intensities of the resonance lines of neutral and ionized magnesium in stellar spectra
Empirical curves giving the dependence of the equivalent widths of thedoublet 2800 Mg II and the line 2852 Mg I on the spectral class havebeen plotted. Some features of the behavior of these lines in thespectra of stars of the spectral classes A-K have been analyzed. Thelines 2795 Mg II and 2852 Mg I have been used to determine the meanelectron concentration ne(Mg) in the atmospheres of 87 stars of thespectral classes B8-K4.
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Zincirli Prenses |
| Sað Açýklýk: | 00h49m16.13s |
| Yükselim: | +68°28'02.1" |
| Görünürdeki Parlaklýk: | 8.123 |
| Uzaklýk: | 671.141 parsek |
| özdevim Sað Açýklýk: | -7.7 |
| özdevim Yükselim: | -2.5 |
| B-T magnitude: | 8.472 |
| V-T magnitude: | 8.152 |
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