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  Magnetic field and chromospheric activity evolution of HD 75332: a rapid magnetic cycle in an F star without a hot Jupiter

Brown, E. L., Marsden, S. C., Mengel, M. W., Jeffers, S. V., Millburn, I., Mittag, M., et al. (2021). Magnetic field and chromospheric activity evolution of HD 75332: a rapid magnetic cycle in an F star without a hot Jupiter. Monthly Notices of the Royal Astronomical Society, 501(3), 3981-4003. doi:10.1093/mnras/staa3878.

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Other : Magnetic field and chromospheric activity evolution of HD75332: a rapid magnetic cycle in an F star without a hot Jupiter


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Brown, E L, Author
Marsden, S C, Author
Mengel, M W, Author
Jeffers, Sandra V.1, Author           
Millburn, I, Author
Mittag, M, Author
Petit, P, Author
Vidotto, A A, Author
Morin, J, Author
See, V, Author
Jardine, M, Author
González-Pérez, J N, Author
The BCool Collaboration, Author              
1Department Solar and Stellar Interiors, Max Planck Institute for Solar System Research, Max Planck Society, Justus-von-Liebig-Weg 3, 37077 Göttingen, DE, ou_1832287              


Free keywords: stars: activity, stars: magnetic field, stars: individual (HD 75332)
 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.


Language(s): eng - English
 Dates: 2021
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa3878
ADS: 2021MNRAS.501.3981B
arXiv: 2012.05407
 Degree: -



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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 501 (3) Sequence Number: - Start / End Page: 3981 - 4003 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150