{
  "id": "2412.18098",
  "version": "v1",
  "published": "2024-12-24T02:15:19.000Z",
  "updated": "2024-12-24T02:15:19.000Z",
  "title": "Bar instability and formation timescale across Toomre's $Q$ parameter and central mass concentration: slow bar formation or true stability",
  "authors": [
    "Tirawut Worrakitpoonpon"
  ],
  "comment": "18 pages, 9 figures, 1 table, accepted for publication in ApJ",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "We investigate the bar formation process using $N$-body simulations across the Toomre's parameter $Q_{min}$ and central mass concentration (CMC), focusing principally on the formation timescale. Of importance is that, as suggested by cosmological simulations, disk galaxies have limited time of $\\sim 8$ Gyr in the Universe timeline to evolve secularly, starting when they became physically and kinematically steady to prompt the bar instability. By incorporating this time limit, bar-unstable disks are further sub-divided into those that establish a bar before and after that time, namely the normal and the slowly bar-forming disks. Simulations demonstrate that evolutions of bar strengths and configurations of the slowly bar-forming and the bar-stable cases are nearly indistinguishable prior to $8$ Gyr, albeit dynamically distinct, while differences can be noticed afterwards. Differentiating them before $8$ Gyr is possible by identifying the proto-bar, a signature of bar development visible in kinematical maps such as the Fourier spectrogram and the angular velocity field, which emerges in the former group $1-2$ Gyr before the fully developed bar, whereas it is absent in the latter group until $8$ Gyr and such bar-stable disk remains unbarred until at least $10$ Gyr. In addition, we find complicated interplays between $Q_{min}$ and CMC in regulating the bar formation. Firstly, disk stabilization requires both high $Q_{min}$ and CMC. Either high $Q_{min}$ or high CMC only results in slow bar formation. Secondly, some hot disks can form a bar more rapidly than the colder ones in a specific range of $Q_{min}$ and CMC.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2024-12-24T02:15:19.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "slow bar formation",
      "central mass concentration",
      "formation timescale",
      "bar instability",
      "true stability"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 18,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}