FCAPT<i>uvby</i>Photometry of the mCP Stars HR 1297, 25 Sex, BX Boo, and 49 Her

Adelman, Saul J.

doi:10.1086/588680

Cited by 7 publications

(7 citation statements)

References 24 publications

(26 reference statements)

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“…For HD 26571, Catalano & Renson (1998) gave a period of 1.06 d, while Renson & Catalano (2001) gave a period of 15.749 d. Our periodogram did not show any significant peak around the 1‐d period; therefore, we presume that the 15.749‐d period, given by Renson & Catalano (2001), is the correct one. Adelman (2008) confirmed the longer period and refined it to 15.7505 d. For HD 134214, Catalano & Renson (1998) gave a period of 248 d, while Renson & Catalano (2001) gave a period of 4.15 d. Our periodogram did not present any significant peak around 4 d, meaning that the longer period is more likely to be the correct one.…”

Section: Resultssupporting

confidence: 62%

“…Our periodogram did not show any significant peak around the 1 day period, therefore we presume that the 15.749 days period, given by Renson & Catalano (2001) is the correct one. Adelman (2008) confirmed the longer period and refined it to 15.7505 days. For HD 134214, Catalano & Renson (1998) gave a period of 248 days, while Renson & Catalano (2001) gave a period of 4.15 days.…”

Section: Notes On Individual Starsmentioning

confidence: 81%

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A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars★

Wraight¹,

Fossati²,

Netopil³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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About 10 per cent of upper main‐sequence stars are characterized by the presence of chemical peculiarities, often found together with a structured magnetic field. The atmospheres of most of those chemically peculiar stars present surface spots, leading to photometric variability caused by rotational modulation. The study of the light curves of those stars therefore permits a precise measurement of their rotational period, which is important to study stellar evolution and to plan further detailed observations. We analysed the light curves of 1028 chemically peculiar stars obtained with the STEREO spacecraft. We present here the results obtained for the 337 magnetic chemically peculiar stars in our sample. Thanks to the cadence and stability of the photometry, STEREO data are perfectly suitable to study variability signals with a periodicity typical of magnetic chemically peculiar stars. Using a matched filter algorithm and then two different period searching algorithms, we compiled a list of 82 magnetic chemically peculiar stars for which we measured a reliable rotational period; for 48 of them, this is the first measurement of their rotational period. The remaining 255 stars are likely to be constant, although we cannot exclude the presence of long‐period variability. In some cases, the presence of blending or systematic effects prevented us from detecting any reliable variability and in those cases we classified the star as constant. For each star we classified as variable, we determined temperature, luminosity, mass and fractional age, but the limited statistics, biased towards the shorter periods, prevented us from finding any evolutionary trend of the rotational period. For a few stars, the comparison between their projected rotational velocity and equatorial velocity let us believe that their real rotational period might be longer than that found here and previously obtained. For the 82 stars identified as variable, we give all necessary information needed to plan further phase‐dependent observations.

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Section: Resultssupporting

confidence: 62%

Section: Notes On Individual Starsmentioning

confidence: 81%

A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars★

Wraight¹,

Fossati²,

Netopil³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…This star is confirmed as a slow rotator with P rot = 15.7505 ± 0.0004 d via ground-based photometry (Adelman 2008) and has a projected surface rotational velocity of v sin i = 20.0 ± 3.0 km s −1 (Wraight et al 2012). However, the rotation period of HD 26571 is somewhat disputed in the literature, where a value of 1.06 d was given by Catalano & Renson (1998), although these authors commented that this value is dubious and could arise from a 1-day alias, and Wraight et al (2012) classifying the star as non-variable.…”

Section: Epic 210964459 -Hd 26571mentioning

confidence: 82%

K2 space photometry reveals rotational modulation and stellar pulsations in chemically peculiar A and B stars

Bowman

Buysschaert

Neiner

et al. 2018

A&A

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Context. The physics of magnetic hot stars and how a large-scale magnetic field affects their interior properties is largely unknown. Few studies have combined high-quality observations and modelling of magnetic pulsating stars, known as magneto-asteroseismology, primarily because of the dearth of detected pulsations in stars with a confirmed and well-characterised large-scale magnetic field. Aims. We aim to characterise observational signatures of rotation and pulsation in chemically peculiar candidate magnetic stars using photometry from the K2 space mission. Thus, we identify the best candidate targets for ground-based, optical spectropolarimetric follow-up observations to confirm the presence of a large-scale magnetic field. Methods. We employed customised reduction and detrending tools to process the K2 photometry into optimised light curves for a variability analysis. We searched for the periodic photometric signatures of rotational modulation caused by surface abundance inhomogeneities in 56 chemically peculiar A and B stars. Furthermore, we searched for intrinsic variability caused by pulsations (coherent or otherwise) in the amplitude spectra of these stars. Results. The rotation periods of 38 chemically peculiar stars are determined, 16 of which are the first determination of the rotation period in the literature. We confirm the discovery of high-overtone roAp pulsation modes in HD 177765 and find an additional 3 Ap and Bp stars that show evidence of high-overtone pressure modes found in roAp stars in the form of possible Nyquist alias frequencies in their amplitude spectra. Furthermore, we find 6 chemically peculiar stars that show evidence of intrinsic variability caused by gravity or pressure pulsation modes. Conclusions. The discovery of pulsations in a non-negligible fraction of chemically peculiar stars make these stars high-priority targets for spectropolarimetric campaigns to confirm the presence of their expected large-scale magnetic field. The ultimate goal is to perform magneto-asteroseismology and probe the interior physics of magnetic pulsating stars.

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“…HD 133029: The 2.8804(3) d TESS period provides a poor phasing of the Bz measurements. The period from Adelman (2008) is similar (2.88756 d), but more precise, and while it does phase the individual Bz datasets this period does not phase the combined DAO and Borra & Landstreet (1980) magnetic datasets. The nearest period which approximately phases Bz is 2.88767(6) d, which also gives a coherent phasing of the TESS and Hipparcos photometry, although this does not result in a perfect match in Bz (see Fig.…”

Section: Starmentioning

confidence: 81%

MOBSTER -- VI. The crucial influence of rotation on the radio magnetospheres of hot stars

Shultz,

Owocki,

ud-Doula

et al. 2022

Preprint

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Numerous magnetic hot stars exhibit gyrosynchrotron radio emission. The source electrons were previously thought to be accelerated to relativistic velocities in the current sheet formed in the middle magnetosphere by the wind opening magnetic field lines. However, a lack of dependence of radio luminosity on the wind power, and a strong dependence on rotation, has recently challenged this paradigm. We have collected all radio measurements of magnetic early-type stars available in the literature. When constraints on the magnetic field and/or the rotational period are not available, we have determined these using previously unpublished spectropolarimetric and photometric data. The result is the largest sample of magnetic stars with radio observations that has yet been analyzed: 131 stars with rotational and magnetic constraints, of which 50 are radio-bright. We confirm an obvious dependence of gyrosynchrotron radiation on rotation, and furthermore find that accounting for rotation neatly separates stars with and without detected radio emission. There is a close correlation between Hα emission strength and radio luminosity. These factors suggest that radio emission may be explained by the same mechanism responsible for Hα emission from centrifugal magnetospheres, i.e. centrifugal breakout (CBO), however, whereas the Hα-emitting magnetosphere probes the cool plasma before breakout, radio emission is a consequence of electrons accelerated in centrifugally-driven magnetic reconnection.

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

Cited by 7 publications

References 24 publications

A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars★

A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars★

K2 space photometry reveals rotational modulation and stellar pulsations in chemically peculiar A and B stars

MOBSTER -- VI. The crucial influence of rotation on the radio magnetospheres of hot stars

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