{
  "id": "2412.05401",
  "version": "v1",
  "published": "2024-12-06T19:57:55.000Z",
  "updated": "2024-12-06T19:57:55.000Z",
  "title": "Rotational Velocities and Radii Estimates of Low-Mass Pre-Main Sequence Stars in NGC 2264",
  "authors": [
    "Laurin M. Gray",
    "Katherine L. Rhode",
    "Catrina M. Hamilton-Drager",
    "Tiffany Picard",
    "Luisa M. Rebull"
  ],
  "comment": "23 pages, 8 figures. Accepted for publication in The Astrophysical Journal",
  "doi": "10.3847/1538-4357/ad924b",
  "categories": [
    "astro-ph.SR",
    "astro-ph.EP",
    "astro-ph.GA"
  ],
  "abstract": "Investigating the angular momentum evolution of pre-main sequence (PMS) stars provides important insight into the interactions between Sun-like stars and their protoplanetary disks, and the timescales that govern disk dissipation and planet formation. We present projected rotational velocities (v sin i values) of 254 T Tauri stars (TTSs) in the ~3 Myr-old open cluster NGC 2264, measured using high-dispersion spectra from the WIYN 3.5m telescope's Hydra instrument. We combine these with literature values of temperature, rotation period, luminosity, disk classification, and binarity. We find some evidence that Weak-lined TTSs may rotate faster than their Classical TTS counterparts and that stars in binary systems may rotate faster than single stars. We also combine our v sin i measurements with rotation period to estimate the projected stellar radii of our sample stars, and then use a maximum likelihood modeling technique to compare our radii estimates to predicted values from stellar evolution models. We find that starspot-free models tend to underestimate the radii of the PMS stars at the age of the cluster, while models that incorporate starspots are more successful. We also observe a mass dependence in the degree of radius inflation, which may be a result of differences in the birthline location on the HR diagram. Our study of NGC 2264 serves as a pilot study for analysis methods to be applied to four other clusters ranging in age from 1 to 14 Myr, which is the timescale over which protoplanetary disks dissipate and planetary systems begin to form.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2024-12-06T19:57:55.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "low-mass pre-main sequence stars",
      "rotational velocities",
      "radii estimates",
      "5m telescopes hydra instrument",
      "rotate faster"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 23,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}