{
  "id": "2308.00764",
  "version": "v1",
  "published": "2023-08-01T18:03:56.000Z",
  "updated": "2023-08-01T18:03:56.000Z",
  "title": "Mode coupling coefficients between the convective core and radiative envelope of $γ\\,$Doradus and slowly pulsating B stars",
  "authors": [
    "Conny Aerts",
    "Stéphane Mathis"
  ],
  "comment": "Manuscript in press at A&A, 9 pages, 8 figures",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "Signatures of coupling between an inertial mode in the convective core and a gravito-inertial mode in the envelope have been found in four-year Kepler light curves of 16 rapidly rotating $\\gamma\\,$Doradus ($\\gamma\\,$Dor) stars. This makes it possible to obtain a measurement of the rotation frequency in their convective core. Despite their similar internal structure and available data, inertial modes have not yet been reported for slowly pulsating B (SPB) stars. We aim to provide a numerical counterpart of the recently published theoretical expressions for the mode-coupling coefficients, $\\varepsilon$ and $\\tilde{\\varepsilon}$. These coefficients represent the two cases of a continuous and a discontinuous Brunt-V\\\"ais\\\"al\\\"a frequency profile at the core-envelope interface, respectively. We used asteroseismic forward models of two samples consisting of 26 SPB stars and 37 $\\gamma\\,$Dor stars to infer their numerical values of $\\varepsilon$. The asteroseismically inferred values of $\\varepsilon$ for the two samples are between 0.0 and 0.34. While $\\varepsilon$ is most strongly correlated with the near-core rotation frequency for $\\gamma\\,$Dor stars, the fractional radius of the convective core instead provides the tightest correlation for SPB stars. We find $\\varepsilon$ to decrease mildly as the stars evolve. Our asteroseismic results for the mode coupling support the theoretical interpretation and reveal that young, fast-rotating $\\gamma\\,$Dor stars are most suitable for undergoing couplings between inertial modes in the rotating convective core and gravito-inertial modes in the radiative envelope. The phenomenon has been found in 2.4\\% of such pulsators with detected period spacing patterns, whereas it has not been seen in any of the SPB stars so far. (shortened abstract to meet the arXiv limits)",
  "revisions": [
    {
      "version": "v1",
      "updated": "2023-08-01T18:03:56.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "convective core",
      "mode coupling coefficients",
      "radiative envelope",
      "slowly pulsating",
      "spb stars"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 9,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}