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

Adelman, Saul J.

doi:10.1051/aas:2000261

Cited by 15 publications

(4 citation statements)

References 8 publications

(10 reference statements)

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“…In the phase diagrams of these two objects, the long-term trend was subtracted from the data. These two stars may be similar in some ways to HR 1297, a B9 Si star, for which periods of 1.06457 days and 15.749 days were reported by Adelman (2000). The astrophysical reason for this behaviour remains unknown but it is certainly connected to the highly variable properties of the stellar photosphere.…”

Section: Time Series Analysissupporting

confidence: 57%

A photometric long-term study of chemically peculiar stars in open clusters

Paunzen

Hensberge

Maitzen

et al. 2010

A&A

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Context. Photometric variability of chemically peculiar (CP) stars of the upper main sequence is closely connected to their local stellar magnetic field and their rotational period. Long term investigations, as presented here, help us to identify possible stellar cycles (as in the Sun). Furthermore, these data provide a basis for detailed surface mapping techniques. Aims. Photoelectric Strömgren uvby time series for 27 CP stars within the boundaries of open clusters are presented. In addition, Hipparcos photometric data (from 1989 to 1993) are used for our analysis. Our observations cover a time period of about six years (1986 to 1992) with typically fifteen measurements for each objects. These observations help us to determine the rotational periods of these objects. Methods. A standard reduction procedure was applied to the data. When possible, we merged our data sets with already published ones to obtain a more significant result. A detailed time series analysis was performed, involving five different methods to minimize spurious detections. Results. We established, for the first time, variability for fourteen CP stars. For additional two stars, a merging of already published data sets, resulted in more precise periods, whereas for six objects, the published periods could be confirmed. Last, but not least, no significant variations were found for five stars. Apart from six stars, all targets seem to be members of their host open clusters. Conclusions. The present observations fill an important gap in previous photometric long-time studies of CP stars. The presented open cluster members are excellent targets for follow-up observations, employing for example polarimetric, high-resolution spectroscopic, and surface mapping techniques.

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Section: Time Series Analysissupporting

confidence: 57%

A photometric long-term study of chemically peculiar stars in open clusters

Paunzen

Hensberge

Maitzen

et al. 2010

A&A

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“…Adelman & Fried (1993) noted that their uvby and UBV photometry of 56 Ari were somewhat different from that previously published. Further both 20 Eri (Adelman & Boyce 1995;Adelman 2000) and 108 Aqr (Adelman & Knox 1994;Adelman 1997Adelman , 1999 show similar behaviors. For these stars, there appear to be two periods of variability, one…”

Section: Introductionmentioning

confidence: 89%

On the rotation of the chemically peculiar magnetic star 56 Arietis

Adelman

Malanushenko

Ryabchikova

et al. 2001

A&A

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Abstract. This study used extensive sets of phase resolved photometric and spectroscopic data obtained by the authors and supplemented by that from the literature to investigate the light and equivalent width variations of the mCP star 56 Ari. Its rotational period is found to be increasing at a rate of about 2 s per 100 years. In addition there is evidence for a second period whose length is about 5 years which is attributed to the precession of the axis of rotation.

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“…On the basis of a precise Four College Photometric Telescope uvby photometry several other mCP stars were revealed with light curves also indicating precession (see the review paper by Pyper & Adelman, 2004): e. g. 108 Aqr (Adelman, 1997b), 20 Eri (Adelman, 2000) man, 2004), MW Vul (Adelman & Young, 2005). As the changes of their periods are marginal (if any), we do not include them among the stars with unsteady rotation.…”

Section: Silicon Mcp Star Sx Arietismentioning

confidence: 99%

Magnetic Chemically Peculiar Stars with Unsteady Periods

Mikulasek,

Krticka,

Janik

et al. 2011

Preprint

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Photometrically and spectroscopically variable chemically peculiar (CP) stars are the optimum laboratories for testing the rotational evolution of main sequence stars. A vast majority of well-studied CP stars have quite steady rotational periods (e. g. SrCrEu star CQ UMa). However, there are several CP stars that exhibit apparent period variations. The origin of the period variations is unclear in many cases. We describe the observed period variations of several individual CP stars, especially V901 Ori, σ Ori E, HR 7355, CU Vir, SX Ari, and EE Dra. The CP stars with unsteady periods now represent a very diverse group with dissimilar O-C diagrams and time scales. We also discuss the causes of the period changes found and a possible cyclicity or chaoticity of them.

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

Cited by 15 publications

References 8 publications

A photometric long-term study of chemically peculiar stars in open clusters

A photometric long-term study of chemically peculiar stars in open clusters

On the rotation of the chemically peculiar magnetic star 56 Arietis

Magnetic Chemically Peculiar Stars with Unsteady Periods

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