Insights from Asteroseismology of Massive Stars: The Need for Additional Angular Momentum Transport Mechanisms

Abstract

In massive stars, rotation and oscillatory waves can have a tight interplay. In order to assess the importance of additional angular momentum transport mechanisms other than rotation, we compare the asteroseismic properties of a uniformly rotating model and a differentially rotating one. Accordingly, we employ the observed period spacing of 36 dipole g-modes in the Kepler $\sim 3.2$ M${}_{\odot }$ target KIC 7760680 to discriminate between these two models. We favor the uniformly rotating model, which fully satisfies all observational constraints. Therefore, efficient angular momentum transport by additional mechanisms such as internal gravity waves, heat-driven modes and magnetic field is needed during early main sequence evolution of massive stars.

Proceedings of "Seismology of the Sun and the Distant Stars 2016". Editors: Mário J. P. F. G. Monteiro, Margarida S. Cunha, João Miguel T. Ferreira

References in corpus (4)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Asteroseismic measurement of surface-to-core rotation in a main sequence A star, KIC 11145123
• Asteroseismic measurement of slow, nearly-uniform surface-to-core rotation in the main sequence F star KIC 9244992
• KIC 10526294: a slowly rotating B star with rotationally split, quasi-equally spaced gravity modes

Cited by in corpus (1)

• Black hole spins in coalescing binary black holes