期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 517, 期 4, 页码 5340-5357出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac2799
关键词
stars: chemically peculiar; stars: fundamental parameters; stars: individual: HD 10840, HD 22920, HD 24712, HD 38170, HD 63401, HD 74521, HD 77314, HD 86592; stars: magnetic field; stars: rotation
资金
- Faculte des Etudes Superieures et de la Recherch
- Natural Sciences and Engineering Research Council of Canada (NSERC)
- NASA [80GSFC21M0002]
- Research Foundation Flanders (FWO) [1286521N]
- Annie Jump Cannon Fellowship - University of Delaware
- NASA Explorer Program
- Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]
- TESS
- TASC/TASOC teams
- Research Foundation - Flanders (FWO), Belgium
- Research Council of KU Leuven, Belgium
- Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium
- Royal Observatory of Belgium
- Observatoire de Geneve, Switzerland
- Thuringer Landessternwarte Tautenburg, Germany
This study used TESS data to investigate the rotational periods of chemically peculiar stars, and found that the critical rotational fractions decrease with stellar age.
Since the end of 2018, the Transiting Exoplanet Survey Satellite (TESS) has provided stellar photometry to the astronomical community. We have used TESS data to study rotational modulation in the light curves of a sample of chemically peculiar stars with measured large-scale magnetic fields (mCP stars). In general, mCP stars show inhomogeneous distributions of elements in their atmospheres that lead to spectroscopic (line profile) and photometric (light curve) variations commensurate with the rotational period. We analyzed the available TESS data from 50 sectors for eight targets after post-processing them in order to minimize systematic instrumental trends. Analysis of the light curves allowed us to determine rotational periods for all eight of our targets. For each star, we provide a phase diagram calculated using the derived period from the light curves and from the available measurements of the disc-averaged longitudinal magnetic field < B-z >. In most cases, the phased light curve and < B-z > measurements show consistent variability. Using our rotation periods, and global stellar parameters derived from fitting Balmer line profiles, and from Geneva and Stromgren-Crawford photometry, we determined the equatorial rotational velocities and calculated the respective critical rotational fractions v(eq)/v(crit). We have shown from our sample that the critical rotational fraction decreases with stellar age, at a rate consistent with the magnetic braking observed in the larger population of mCP stars.
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