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

Author:

Brown E L1ORCID,Marsden S C1,Mengel M W1ORCID,Jeffers S V2,Millburn I1ORCID,Mittag M3,Petit P4,Vidotto A A5ORCID,Morin J6,See V7ORCID,Jardine M8ORCID,González-Pérez J N3,

Affiliation:

1. Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD 4350, Australia

2. Max Planck Institut for Solar System Research, Justus-von-Liebig-Weg 3, D-37077 Göttingen, Germany

3. Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany

4. IRAP (Institut de Recherche en Astrophysique et Planétologie), Université de Toulouse, CNRS, CNES, UPS, 14 Avenue Edouard Belin, F-31400 Toulouse, France

5. School of Physics, Trinity College Dublin, The University of Dublin, College Green, Dublin-2, D02 PN40 Ireland

6. LUPM, Université de Montpellier, CNRS, Place Eugéne Bataillon, F-34095 Montpellier, France

7. Department of Physics & Astronomy, University of Exeter, Stoker Road, Devon, Exeter EX4 4QL, UK

8. SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK

Abstract

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.

Funder

National Aeronautics and Space Administration

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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