Hydrodynamical simulations of mixed modes in evolved low-mass stars

Low-mass evolved stars exhibit a phenomenon known as mixed modes, which originate from the coupling of sound waves in the convective envelope to internal gravity waves in the radiative interior. One can therefore probe features of the deep interior, such as the core rotation rate, from the signatures of the mixed modes at the surface of evolved stars. So far, many observations of mixed modes have been made using CoRoT, Kepler, and TESS, but they have not yet been identified in hydrodynamical simulations. I will present the first simulation revealing the presence of mixed modes in a 1.3M⊙ fully compressible evolved star model. Furthermore, I will attempt to obtain the amplitudes of the mixed modes in our simulations, in an effort to constrain the resulting angular momentum transport, thought to be one of the explanations for the smaller than expected difference in rotation rates between the core and envelope.