%0 Journal Article
%T Monitoring the large-scale magnetic field of AD Leo with SPIRou, ESPaDOnS, and Narval
%T Towards a magnetic polarity reversal?
%+ Institut de recherche en astrophysique et planétologie (IRAP)
%+ ESA - ESTEC (Netherlands)
%+ Laboratoire Univers et Particules de Montpellier (LUPM)
%+ University of Tartu
%+ Institut de Planétologie et d'Astrophysique de Grenoble (IPAG)
%+ Institut d'Astrophysique de Paris (IAP)
%+ Laboratorio Nacional de Astrofisica
%+ Universidade Federal de Minas Gerais = Federal University of Minas Gerais [Belo Horizonte, Brazil] (UFMG)
%+ Université de Montréal (UdeM)
%+ Laboratoire d'Astrophysique de Marseille (LAM)
%+ Observatoire Astronomique de l'Université de Genève (ObsGE)
%+ McMaster University [Hamilton, Ontario]
%+ Uppsala University
%+ Royal Military College of Canada (RMCC)
%A Bellotti, S.
%A Morin, Julien
%A Lehmann, L. T.
%A Folsom, C. P.
%A Hussain, G. A. J.
%A Petit, P.
%A Donati, J-F
%A Lavail, A.
%A Carmona, A.
%A Martioli, E.
%A Romano Zaire, B.
%A Alecian, Evelyne
%A Moutou, C.
%A Fouqué, P
%A Alencar, S.
%A Artigau, E.
%A Boisse, I.
%A Bouchy, F.
%A Cadieux, C.
%A Cloutier, R.
%A Cook, N, J
%A Delfosse, X.
%A Doyon, R.
%A Hébrard, G
%A Kochukhov, O.
%A Wade, G, A
%< avec comité de lecture
%@ 0004-6361
%J Astronomy and Astrophysics - A&A
%I EDP Sciences
%V 676
%P A56
%8 2023
%D 2023
%Z 2307.01016
%Z 2023A&A...676A..56B
%R 10.1051/0004-6361/202346845
%K Stars: individual: AD Leo
%K Stars: magnetic field
%K Stars: activity
%K Techniques: polarimetric
%K Stars: individual: AD Leo
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]Journal articles
%X Context. One clear manifestation of dynamo action on the Sun is the 22-yr magnetic cycle, exhibiting a polarity reversal and a periodic conversion between poloidal and toroidal fields. For M dwarfs, several authors claim evidence of activity cycles from photometry and analyses of spectroscopic indices, but no clear polarity reversal has been identified from spectropolarimetric observations. These stars are excellent laboratories to investigate dynamo-powered magnetic fields under different stellar interior conditions, that is partly or fully convective.Aims. Our aim is to monitor the evolution of the large-scale field of AD Leo, which has shown hints of a secular evolution from past dedicated spectropolarimetric campaigns. This is of central interest to inform distinct dynamo theories, contextualise the evolution of the solar magnetic field, and explain the variety of magnetic field geometries observed in the past.Methods. We analysed near-infrared spectropolarimetric observations of the active M dwarf AD Leo taken with SPIRou between 2019 and 2020 and archival optical data collected with ESPaDOnS and Narval between 2006 and 2019. We searched for longterm variability in the longitudinal field, the width of unpolarised Stokes profiles, the unsigned magnetic flux derived from Zeeman broadening, and the geometry of the large-scale magnetic field using both Zeeman-Doppler imaging and principal component analysis.Results. We found evidence of a long-term evolution of the magnetic field, featuring a decrease in axisymmetry (from 99% to 60%). This is accompanied by a weakening of the longitudinal field (−300 to −50 G) and a correlated increase in the unsigned magnetic flux (2.8 to 3.6 kG). Likewise, the width of the mean profile computed with selected near-infrared lines manifests a long-term evolution corresponding to field strength changes over the full time series, but does not exhibit modulation with the stellar rotation of AD Leo in individual epochs.Conclusions. The large-scale magnetic field of AD Leo manifested first hints of a polarity reversal in late 2020 in the form of a substantially increased dipole obliquity, while the topology remained predominantly poloidal and dipolar for 14 yr. This suggests that low-mass M dwarfs with a dipole-dominated magnetic field can undergo magnetic cycles.
%G English
%Z SPIRou Legacy Survey
%2 https://hal.science/hal-04187255/document
%2 https://hal.science/hal-04187255/file/aa46845-23.pdf
%L hal-04187255
%U https://hal.science/hal-04187255
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