---
author:
- 'T. Van Reeth'
- 'A. Tkachenko'
- 'C. Aerts'
bibliography:
- 'Rotation\_paper.bib'
date: 'Received / Accepted'
title: 'The interior rotation of a sample of $\gamma$ Doradus stars from ensemble modelling of their gravity mode period spacings[^1]'
---

Introduction {#sec:intro}
============

Gamma Dor stars are early F- to late A-type stars (with $1.4\,M_\odot \lesssim M
\lesssim 2.0\,M_\odot$) which exhibit non-radial gravity and/or gravito-inertial mode pulsations [e.g. @Kaye1999]. This places them directly within the transition region between low-mass stars with a convective envelope and intermediate-mass stars with a convective core, where the CNO-cycle becomes increasingly important relative to the pp-chain as the dominant hydrogen burning mechanism [e.g. @Silva2011]. The pulsations in $\gamma$Dor stars are excited by the flux blocking mechanism at the bottom of the convective envelope [@Guzik2000; @Dupret2005], though the $\kappa$ mechanism has been linked to $\gamma$Dor type pulsations as well [@Xiong2016]. The oscillations predominantly trace the radiative region near the convective core boundary. As a result these pulsators are ideal to characterise the structure of the deep stellar interior.

As shown by @Tassoul1980, high order ($n \gg l$) gravity modes are asymptotically equidistant in period for non-rotating chemically homogeneous stars with a convective core and a radiative 