The determination of the rotational periods of rapidly oscillating AP stars from their mean light variations. II - HR 1217 (HD 24712)

Details The determination of the rotational periods of rapidly oscillating AP stars from their mean light variations. II - HR 1217 (HD 24712) The determination of the rotational periods of rapidly oscillating AP stars from their mean light variations. II - HR 1217 (HD 24712)

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.229..285k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 229, Nov. 15, 1987, p. 285-293. Research supported by t

Other

23

A Stars, Peculiar Stars, Periodic Variations, Stellar Luminosity, Stellar Oscillations, Stellar Rotation, Line Spectra, Stellar Spectrophotometry, Ubv Spectra

Scientific paper

The authors have obtained new UBVRI mean light observations of HR 1217 in 1986 and 1987. A frequency analysis of the new B observations along with previous B observations, Strömgren b observations and Eu II line strength observations leads unambiguously to a revised rotational ephemeris. All of the non-magnetic observations can be fitted with this ephemeris to the accuracy of the data. On the other hand, the magnetic measurements have slightly, but significantly, different times of maxima; magnetic maximum does not occur at exactly the same time as the extrema in the photometric mean light measurements or the Eu II line strength measurements. The phase shift between the photometric and line strengths observations and the magnetic observations is 1.00±0.35 day or 0.080±0.028 periods. The amplitude of the mean light variations decreases monotonically as a function of wavelength for the five bandpasses studied. There is an indication that the phase of the mean light variations may increase as a function of wavelength.

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