One year of AU Mic with HARPS – II. Stellar activity and star–planet interaction

• Published in: Monthly notices of the Royal Astronomical Society Vol. 512; no. 4; pp. 5067 - 5084
• Main Authors: Klein, Baptiste, Zicher, Norbert, Kavanagh, Robert D, Nielsen, Louise D, Aigrain, Suzanne, Vidotto, Aline A, Barragán, Oscar, Strugarek, Antoine, Nicholson, Belinda, Donati, Jean-François, Bouvier, Jérôme
• Format: Journal Article
• Language: English
• Published: Oxford University Press 12.04.2022; Oxford University Press (OUP): Policy P - Oxford Open Option A
• Subjects: Astrophysics; Sciences of the Universe; planet and satellites: formation; stars: individual: AU Microscopii; stars: imaging; stars: activity
• DOI: 10.1093/mnras/stac761
• ISSN: 0035-8711

ABSTRACT We present a spectroscopic analysis of a 1-yr intensive monitoring campaign of the 22-Myr old planet-hosting M dwarf AU Mic using the HARPS spectrograph. In a companion paper, we reported detections of the planet radial velocity (RV) signatures of the two close-in transiting planets of the system, with respective semi-amplitudes of 5.8 ± 2.5 and 8.5 ± 2.5 m s−1 for AU Mic b and AU Mic c. Here, we perform an independent measurement of the RV semi-amplitude of AU Mic c using Doppler imaging to simultaneously model the activity-induced distortions and the planet-induced shifts in the line profiles. The resulting semi-amplitude of 13.3 ± 4.1 m s−1 for AU Mic c reinforces the idea that the planet features a surprisingly large inner density, in tension with current standard models of core accretion. Our brightness maps feature significantly higher spot coverage and lower level of differential rotation than the brightness maps obtained in late 2019 with the SPIRou spectropolarimeter, suggesting that the stellar magnetic activity has evolved dramatically over a ∼1-yr time span. Additionally, we report a 3σ detection of a modulation at 8.33 ± 0.04 d of the He i D3 (5875.62 Å) emission flux, close to the 8.46-d orbital period of AU Mic b. The power of this emission (a few 1017 W) is consistent with 3D magnetohydrodynamical simulations of the interaction between stellar wind and the close-in planet if the latter hosts a magnetic field of ∼10 G. Spectropolarimetric observations of the star are needed to firmly elucidate the origin of the observed chromospheric variability.