Magnetic field and chromospheric activity evolution of HD 75332: a rapid magnetic cycle in an F star without a hot Jupiter
Article
Article Title | Magnetic field and chromospheric activity evolution of HD 75332: a rapid magnetic cycle in an F star without a hot Jupiter |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Brown, E. L. (Author), Marsden, S. C. (Author), Mengel, M. W. (Author), Jeffers, S. V. (Author), Millburn, I. (Author), Mittag, M. (Author), Petit, P. (Author), Vidotto, A. A. (Author), Morin, J. (Author), See, V. (Author), Jardine, M. (Author) and Gonzalez-Perez, J. N. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 501 (3), pp. 3981-4003 |
Number of Pages | 23 |
Year | 2020 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/staa3878 |
Web Address (URL) | https://academic.oup.com/mnras/article/501/3/3981/6041709 |
Abstract | Studying cool star magnetic activity gives an important insight into the stellar dynamo and its relationship with stellar properties, as well as allowing us to place the Sun's magnetism in the context of other stars. Only 61 Cyg A (K5V) and τ Boo (F8V) are currently known to have magnetic cycles like the Sun's, where the large-scale magnetic field polarity reverses in phase with the star's chromospheric activity cycles. τ Boo has a rapid ~240 d magnetic cycle, and it is not yet clear whether this is related to the star's thin convection zone or if the dynamo is accelerated by interactions between τ Boo and its hot Jupiter. To shed light on this, we studied the magnetic activity of HD 75332 (F7V) which has similar physical properties to τ Boo and does not appear to host a hot Jupiter. We characterized its long-term chromospheric activity variability over 53 yr and used Zeeman Doppler Imaging to reconstruct the large-scale surface magnetic field for 12 epochs between 2007 and 2019. Although we observe only one reversal of the large-scale magnetic dipole, our results suggest that HD 75332 has a rapid ~1.06 yr solar-like magnetic cycle where the magnetic field evolves in phase with its chromospheric activity. If a solar-like cycle is present, reversals of the large-scale radial field polarity are expected to occur at around activity cycle maxima. This would be similar to the rapid magnetic cycle observed for τ Boo, suggesting that rapid magnetic cycles may be intrinsic to late-F stars and related to their shallow convection zones. |
Keywords | stars: Activity; stars: Individual (HD 75332); stars: Magnetic field |
Related Output | |
Is part of | The magnetic fields, activity and hidden companions of solar-type stars |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | This article is part of a UniSQ Thesis by publication. See Related Output. |
File reproduced in accordance with the copyright policy of the publisher/author/creator. | |
Byline Affiliations | Centre for Astrophysics |
Max Planck Society, Germany | |
University of Hamburg, Germany | |
University of Toulouse, France | |
University of Dublin, Ireland | |
University of Montpellier, France | |
University of Exeter, United Kingdom | |
University of St Andrews, United Kingdom | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q703z/magnetic-field-and-chromospheric-activity-evolution-of-hd-75332-a-rapid-magnetic-cycle-in-an-f-star-without-a-hot-jupiter
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