Rotational periods of magnetic chemically peculiar stars
2008
Magnetic chemically peculiar (mCP) stars of the upper part of
the main sequence usually exhibit strictly periodic variations
of their light, spectrum and magnetic field. These changes can
be well explained using the oblique rotator model of the
rigidly rotating star with persistent photometric spots, uneven
horizontal abundance of chemical elements and dipole-like
magnetic field. Long-term observations of mCP stars variability
enable to determine their rotational periods with an
extraordinary accuracy and reliability.
We compare rotational periods of mCP stars with those of normal
main sequence stars of the same spectral type and discuss the
found discrepancies. We also discuss the cases of mCP stars
V901 Ori, SX Ari, CU Vir, (and possibly also EE Dra), which
have been reported to display an increase of their rotational
periods.
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