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The rotation of AP stars
Photometric periods of silicon stars belonging to clusters andassociations as well as to the field are discussed in relation withtheories of magnetic braking taking place on the main sequence. It isshown that Si stars do not lose the bulk of their angular momentumduring their main-sequence lifetime, but must have lost it before. Anybraking mechanism which predicts an e-folding time of the order of, orshorter than, the star's lifetime seems ruled out. The theory of purelyhydromagnetic rotational braking is much too efficient to fit theobservations (unless under its earlier form proposed by Kulsrud, 1971),while the accretion theory does not fit them either, although it seemsmore realistic. Preinjection of cosmic rays by means of Ap stars appearsdoubtful.
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Observation and Astrometry data
| Constellation: | カシオペヤ座 |
| Right ascension: | 00h35m59.64s |
| Declination: | +72°29'55.5" |
| Apparent magnitude: | 8.276 |
| Distance: | 529.101 parsecs |
| Proper motion RA: | -22.2 |
| Proper motion Dec: | -26.2 |
| B-T magnitude: | 10.738 |
| V-T magnitude: | 8.48 |
Catalogs and designations:
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