The classical T Tauri star CI Tau observed with SPIRou: magnetospheric accretion and planetary formation

• Published in: Monthly notices of the Royal Astronomical Society Vol. 530; no. 1; pp. 264 - 286
• Main Authors: Donati, J -F, Finociety, B, Cristofari, P I, Alencar, S H P, Moutou, C, Delfosse, X, Fouqué, P, Arnold, L, Baruteau, C, Kóspál, Á, Ménard, F, Carmona, A, Grankin, K, Takami, M, Artigau, E, Doyon, R, Hébrard, G
• Format: Journal Article
• Language: English
• Published: Oxford University Press 05.04.2024; Oxford University Press (OUP): Policy P - Oxford Open Option A
• Subjects: Sciences of the Universe; stars: formation; stars: imaging; planetary systems; techniques: polarimetric; stars: magnetic fields; stars: individual: CI Tau; CI Tautechniques; magnetic fields -stars; individual; planetary systems -stars; stars; formation -stars; imaging -stars; polarimetric; stars magnetic fields -stars imaging -stars planetary systems -stars formation -stars individual CI Tautechniques polarimetric
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stae675

ABSTRACT We report new observations of the classical T Tauri star CI Tau with the SPIRou near-infrared spectropolarimeter and velocimeter at the Canada–France–Hawaii Telescope (CFHT) in late 2019, 2020, and 2022, complemented with observations obtained with the ESPaDOnS optical spectropolarimeter at CFHT in late 2020. From our SPIRou and ESPaDOnS spectra, to which we applied least-squares deconvolution, we infer longitudinal fields clearly modulated with the 9-d rotation period of CI Tau. Using Zeeman–Doppler imaging, we reconstruct the large-scale magnetic topology, first from SPIRou data only in all three seasons, then from our 2020 SPIRou and ESPaDOnS data simultaneously. We find that CI Tau hosts a mainly axisymmetric poloidal field, with a 1 kG dipole slightly tilted to the rotation axis and dark spots close to the pole that coincide with the footpoints of accretion funnels linking the star to the inner disc. Our results also suggest that CI Tau accretes mass from the disc in a stable fashion. We further find that radial velocities (RVs) derived from atomic and CO lines in SPIRou spectra are both rotationally modulated, but with a much lower amplitude than that expected from the putative candidate planet CI Tau b. We confirm the presence of a RV signal at a period of 23.86 d reported in a separate analysis, but detect it clearly in CO lines only and not in atomic lines, suggesting that it likely traces a non-axisymmetric structure in the inner disc of CI Tau rather than a massive close-in planet.