<i>uvby</i> photometry of the magnetic CP stars 45 Leonis, 
HR 4330,
49 Herculis, and HR 6718

Adelman, Saul J.; Rayle, K. E.; Pi, Chun-Mei

doi:10.1051/aas:1999221

Cited by 17 publications

(11 citation statements)

References 10 publications

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“…Adopting the period P = 2 × 3.5160 = 7.0320 days, our measurements of H eff show a sinusoidal variation. However, with this period there is a small shift between the Adelman et al (1999) and Hipparcos light curves. Thus we have adopted the ephemeris: JD(y max ) = 2 441 447.71 + 7.0286 E that let the Adelman and Hipparcos light curves to vary in phase (Fig.…”

Section: Ep Uma = Hd 96707 = Hr 4330 = Hip 54540mentioning

confidence: 96%

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Spectropolarimetric measurements of the mean longitudinal magnetic field of chemically peculiar stars

Leone

Catanzaro

2001

A&A

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Abstract. For a sample of chemically peculiar stars, we report time-resolved measurements of the effective magnetic field which were obtained with the spectropolarimetry operating at the Catania Astrophysical Observatory. These observations are combined with data from the literature for better pointing out that periodic magnetic variability which characterises this class of stars. Periods given in the literature have been checked and, if possible, redetermined, not only by means of the magnetic measurements but referring also to the Hipparcos photometry. The variability of the effective magnetic field of the already known magnetic star 25 Sex is pointed out for the first time. As to the suspected magnetic chemically peculiar star EP UMa, our measurements confirm that this is really a magnetic star and we indicate a possible variability period. The accuracy of the variability period for CS Vir and FF Vir is improved. The suggestion that light variability is due to the re-distribution of ultraviolet flux towards the visible wavelengths in metal rich regions, which are not homogeneously distributed on the stellar surface, appears not always and straightly valid. Local line-blocking is certainly important in the case of CS Vir and a direct influence of the magnetic field on the infrared photometric variability cannot be ruled out for 25 Sex.

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Section: Ep Uma = Hd 96707 = Hr 4330 = Hip 54540mentioning

confidence: 96%

“…Adelman et al (1999) have obtained Strömgren photometric observations of EP UMa and concluded that this star presents single-wave light variations with a 3.5160 day period. The amplitude is 0.02 mag in b and 0.025 mag in y filter, with those in u and v probably smaller.…”

Section: Ep Uma = Hd 96707 = Hr 4330 = Hip 54540mentioning

confidence: 99%

Spectropolarimetric measurements of the mean longitudinal magnetic field of chemically peculiar stars

Leone

Catanzaro

2001

A&A

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“…He adopted a period of 1.0978 days, but noted that the resonance period of 0.918 days was a possible alternative. Adelman et al (1999) -uvby photometry of 25 SEX for observing seasons 1 (squares), 2 (diamonds). 3 (circles), 4 (upward-pointing triangles), 5 (plus signs), 11 (crosses), and 15 (right-facing triangles) plotted using HJDðtoÞ ¼ 2445659:000 þ ð4:37900 AE 0:00004Þ E The photometry is best described as in phase without seasonal differences.…”

Section: Bx Boomentioning

confidence: 99%

FCAPTuvbyPhotometry of the mCP Stars HR 1297, 25 Sex, BX Boo, and 49 Her

Adelman

2008

PUBL ASTRON SOC PAC

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ABSTRACT. I obtained additional differential Strömgren uvby observations of four magnetic CP stars HR 1297, 25 Sex, BX Boo, and 49 Her with the Four College Automated Photoelectric Telescope (FCAPT). The seasonal light curves of 25 Sex do not show definite differences. The period of Manfroid & Renson of 4.37900 days is confirmed. The other three stars usually have light curves in phase or nearly so, but there are differences between observing seasons. As the local properties of the photosphere change very slowly with time for these stars that have radiative atmospheres and strong magnetic fields, we are viewing slightly different hemispheres at the same phase. To produce this result, their rotational axes precess about their magnetic axes. For HR 1297, which has moderate amplitudes of variation, the period of Adelman is refined to 15.7505 days. The additional observations of BX Boo do not change the best estimate of its period, 2.88756 days. Although its amplitudes of variation are less than those of HR 1297, there are similar differences between observing seasons. For 49 Her the period of 0.93663 days of Adelman et al. is verified. There are probably small season-to-season light curve differences. Of the mCP stars for which I have FCAPT Strömg-ren observations, at least 13% exhibit variability among their light curves for different years.

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“…Photometric studies using data from the FCAPT have both improved periods and better defined the shapes of their light curves (see, e.g. Adelman et al 1999). If spectra of these stars are obtained as a function of rotational phase, the distribution of surface abundances can be derived for stars which show modest to moderate rotation.…”

Section: Introductionmentioning

confidence: 99%

uvby photometry of the magnetic CP stars 20 Eridani, HR 1297, 12 Canis Majoris, and HD 134214

Adelman

2000

Astron. Astrophys. Suppl. Ser.

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uvby photometry of the magnetic CP stars 45 Leonis, HR 4330, 49 Herculis, and HR 6718

Cited by 17 publications

References 10 publications

Spectropolarimetric measurements of the mean longitudinal magnetic field of chemically peculiar stars

Spectropolarimetric measurements of the mean longitudinal magnetic field of chemically peculiar stars

FCAPTuvbyPhotometry of the mCP Stars HR 1297, 25 Sex, BX Boo, and 49 Her

uvby photometry of the magnetic CP stars 20 Eridani, HR 1297, 12 Canis Majoris, and HD 134214

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