Seismic evidence for near solid-body rotation in two Kepler subgiants and implications for angular momentum transport

¹ IRAP, Université de Toulouse, CNRS, CNES, UPS, Toulouse, France
e-mail: sebastien.deheuvels@irap.omp.eu
² Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
³ Max-Planck Institut für Sonnensystemforschung, Justus-von-Liebig Weg 3, 37077 Göttingen, Germany
⁴ Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Konkoly Thege 15-17, 1121 Budapest, Hungary
⁵ ELTE Eötvös Lorànd University, Institute of Physics, Budapest, Hungary

Received: 4 June 2020
Accepted: 1 July 2020

Abstract

Context. Asteroseismic measurements of the internal rotation of subgiants and red giants all show the need for invoking a more efficient transport of angular momentum than theoretically predicted. Constraints on the core rotation rate are available starting from the base of the red giant branch (RGB) and we are still lacking information on the internal rotation of less evolved subgiants.

Aims. We identify two young Kepler subgiants, KIC 8524425 and KIC 5955122, whose mixed modes are clearly split by rotation. We aim to probe their internal rotation profile and assess the efficiency of the angular momentum transport during this phase of the evolution.

Methods. Using the full Kepler data set, we extracted the mode frequencies and rotational splittings for the two stars using a Bayesian approach. We then performed a detailed seismic modeling of both targets and used the rotational kernels to invert their internal rotation profiles using the MOLA inversion method. We thus obtained estimates of the average rotation rates in the g-mode cavity (⟨Ω⟩_g) and in the p-mode cavity (⟨Ω⟩_p).

Results. We found that both stars are rotating nearly as solid bodies, with core-envelope contrasts of ⟨Ω⟩_g/⟨Ω⟩_p = 0.68 ± 0.47 for KIC 8524425 and ⟨Ω⟩_g/⟨Ω⟩_p = 0.72 ± 0.37 for KIC 5955122. This result shows that the internal transport of angular momentum has to occur faster than the timescale at which differential rotation is forced in these stars (between 300 Myr and 600 Myr). By modeling the additional transport of angular momentum as a diffusive process with a constant viscosity ν_add, we found that values of ν_add >  5 × 10⁴ cm² s⁻¹ are required to account for the internal rotation of KIC 8524425, and ν_add >  1.5 × 10⁵ cm² s⁻¹ for KIC 5955122. These values are lower than or comparable to the efficiency of the core-envelope coupling during the main sequence, as given by the surface rotation of stars in open clusters. On the other hand, they are higher than the viscosity needed to reproduce the rotation of subgiants near the base of the RGB.

Conclusions. Our results yield further evidence that the efficiency of the internal redistribution of angular momentum decreases during the subgiant phase. We thus bring new constraints that will need to be accounted for by mechanisms that are proposed as candidates for angular momentum transport in subgiants and red giants.