{
  "id": "2003.11747",
  "version": "v1",
  "published": "2020-03-26T05:29:56.000Z",
  "updated": "2020-03-26T05:29:56.000Z",
  "title": "A White-light Flare Powered by Magnetic Reconnection in the Lower Solar Atmosphere",
  "authors": [
    "Yongliang Song",
    "Hui Tian",
    "Xiaoshuai Zhu",
    "Yajie Chen",
    "Mei Zhang",
    "Jingwen Zhang"
  ],
  "comment": "14 pages,5 figures,accepted for publication by ApJL",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "White-light flares (WLFs), first observed in 1859, refer to a type of solar flares showing an obvious enhancement of the visible continuum emission. This type of enhancement often occurs in most energetic flares, and is usually interpreted as a consequence of efficient heating in the lower solar atmosphere through non-thermal electrons propagating downward from the energy release site in the corona. However, this coronal-reconnection model has difficulty in explaining the recently discovered small WLFs. Here we report a C2.3 white-light flare, which are associated with several observational phenomena: fast decrease in opposite-polarity photospheric magnetic fluxes, disappearance of two adjacent pores, significant heating of the lower chromosphere, negligible increase of hard X-ray flux, and an associated U-shaped magnetic field configuration. All these suggest that this white-light flare is powered by magnetic reconnection in the lower part of the solar atmosphere rather than by reconnection higher up in the corona.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2020-03-26T05:29:56.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "lower solar atmosphere",
      "white-light flare",
      "magnetic reconnection",
      "opposite-polarity photospheric magnetic fluxes",
      "hard x-ray flux"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 14,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}