Monitoring the young planet host V1298 Tau with SPIRou: planetary system and evolving large-scale magnetic field

Author:

Finociety B1ORCID,Donati J-F1ORCID,Cristofari P I2ORCID,Moutou C1,Cadieux C3,Cook N J3,Artigau E3,Baruteau C1ORCID,Debras F1,Fouqué P1,Bouvier J4,Alencar S H P5,Delfosse X4,Grankin K6ORCID,Carmona A4,Petit P1,Kóspál Á7,

Affiliation:

1. IRAP, Université de Toulouse, CNRS , 14 Avenue Belin, F-31400 Toulouse , France

2. Center for Astrophysics | Harvard & Smithsonian , 60 Garden Street, MS-15, Cambridge, MA 02138 , USA

3. IREX, Département de Physique, Université de Montréal , Montréal, QC H3C 3J7 , Canada

4. IPAG, Université Grenoble Alpes, CNRS , F-38000 Grenoble , France

5. Departamento de Fisica - ICEx - UFMG , Avenida Antonio Carlos 6627, 30270-901 Belo Horizonte, MG , Brazil

6. Crimean Astrophysical Observatory , 298409 Nauchny , Republic of Crimea

7. Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences, CSFK, MTA Centre of Excellence , Konkoly-Thege Miklós út 15-17, 1121 Budapest , Hungary

Abstract

ABSTRACT We report results of a spectropolarimetric monitoring of the young Sun-like star V1298 Tau based on data collected with the near-infrared spectropolarimeter SPIRou at the Canada–France–Hawaii Telescope between late 2019 and early 2023. Using Zeeman–Doppler Imaging and the Time-dependent Imaging of Magnetic Stars methods on circularly polarized spectra, we reconstructed the large-scale magnetic topology of the star (and its temporal evolution), found to be mainly poloidal and axisymmetric with an average strength varying from 90 to 170 G over the ∼3.5 yr of monitoring. The magnetic field features a dipole whose strength evolves from 85 to 245 G, and whose inclination with respect to the stellar rotation axis remains stable until 2023 where we observe a sudden change, suggesting that the field may undergo a polarity reversal, potentially similar to those periodically experienced by the Sun. Our data suggest that the differential rotation shearing the surface of V1298 Tau is about 1.5 times stronger than that of the Sun. When coupling our data with previous photometric results from K2 and TESS and assuming circular orbits for all four planets, we report a 3.9σ detection of the radial velocity signature of the outermost planet (e), associated with a most probable mass, density, and orbital period of $M_\mathrm{e}=0.95^{+0.33}_{-0.24}$ MꝜ, $\rho _\mathrm{e}=1.66^{+0.61}_{-0.48}$$\rm g\, cm^{-3}$, and Pe = 53.0039 ± 0.0001 d, respectively. For the three inner planets, we only derive 99 per cent confidence upper limits on their mass of 0.44, 0.22, and 0.25 MꝜ, for b, c, and d, respectively.

Funder

European Research Council

CNPq

CAPES

FAPEMIG

ANR

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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