{
  "id": "2411.19741",
  "version": "v1",
  "published": "2024-11-29T14:40:11.000Z",
  "updated": "2024-11-29T14:40:11.000Z",
  "title": "A New Look at Disk Winds and External Photoevaporation in the $σ$-Orionis Cluster",
  "authors": [
    "K. Maucó",
    "C. F. Manara",
    "A. Bayo",
    "J. Hernández",
    "J. Campbell-White",
    "N. Calvet",
    "G. Ballabio",
    "M. L. Aru",
    "J. M. Alcalá",
    "M. Ansdell",
    "C. Briceño",
    "S. Facchini",
    "T. J. Haworth",
    "M. McClure",
    "J. P. Williams"
  ],
  "comment": "Accepted for publication on Astronomy & Astrophysics. 14 pages, 11 figures + appendix. Abstract abridged to meet arXiv requirements",
  "categories": [
    "astro-ph.SR",
    "astro-ph.EP",
    "astro-ph.GA"
  ],
  "abstract": "Disk winds play a crucial role in the evolution of protoplanetary disks. Typical conditions for star and planet formation are in regions with intermediate or strong UV radiation fields produced by massive stars. The $\\sigma$-Orionis cluster is the ideal site to study disk winds under these conditions; its outer parts can be used to study disk evolution, while its innermost regions to study the effect of external irradiation. For this, we analyze the $\\rm [OI]\\,\\lambda$6300, $\\rm [NII]\\,\\lambda$6583, and $\\rm [SII]\\,\\lambda$6731,$\\lambda$6716 lines using high-resolution MIKE spectra of 27 classical T Tauri stars and complemented by intermediate-resolution X-shooter data. We decompose the line profiles into multiple Gaussian components. We calculated luminosities, line ratios, and kinematic properties of these components. We found that the $\\rm [OI]\\,\\lambda$6300 line luminosity and kinematic properties are similar to those found in low-mass star-forming regions (SFRs). The frequency of single-component $\\rm [OI]\\,\\lambda$6300 line profiles reflects the expected evolutionary stage given the intermediate age of $\\sigma$-Orionis. This points to internal processes contributing to the line emission. However, the highly irradiated disks do not follow the accretion - [OI] luminosity relation found in low-mass SFRs, and all exhibit single-component line profiles. Line ratios of highly ionized species of [NII] and [SII] show higher ratios than typical values found in low-mass SFRs. The innermost regions of $\\sigma$-Orionis are clearly affected by external irradiation, evidenced by the lack of correlation in the accretion - [OI] luminosity relation. The broad line widths of close-in sources, however, indicate a contribution from internal processes, such as magnetohydrodynamical winds and/or internal photoevaporation. This suggests a coevolution of internal and external winds in $\\sigma$-Orionis.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2024-11-29T14:40:11.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "disk winds",
      "orionis cluster",
      "external photoevaporation",
      "line profiles",
      "kinematic properties"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 14,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}