{
  "id": "1912.11572",
  "version": "v1",
  "published": "2019-12-25T01:42:50.000Z",
  "updated": "2019-12-25T01:42:50.000Z",
  "title": "Superflares on solar-type stars from the first year observation of TESS",
  "authors": [
    "Zuo-Lin Tu",
    "Ming Yang",
    "Z. J. Zhang",
    "F. Y. Wang"
  ],
  "comment": "Accepted for Publication in ApJ. Comments are welcome",
  "categories": [
    "astro-ph.SR",
    "astro-ph.EP"
  ],
  "abstract": "Superflares, as strong explosions on stars, have been well studied with the progress of space time-domain astronomy. In this work, we present the study of superflares on solar-type stars using Transiting Exoplanet Survey Satellite ({\\em{TESS}}) data. 13 sectors of observations during the first year of the {\\em TESS} mission have covered the southern hemisphere of the sky, containing 25,734 solar-type stars. We verified 1,216 superflares on 400 solar-type stars through automatic search and visual inspection with 2-minute cadence data. Our result suggests a higher superflare frequency distribution than the result from {\\em Kepler}. The reason may be that the majority of {\\em TESS} solar-type stars in our dataset are rapidly rotating stars. The power-law index $\\gamma$ of the superflare frequency distribution ($dN/dE\\propto E^{-\\gamma}$) is constrained to be $\\gamma = 2.16\\pm 0.10$, which is a little larger than that of solar flares but consistent with the results from {\\em Kepler}. Because only 7 superflares of Sun-like stars are detected, we may not give a robust superflare occurrence frequency. And four stars are accompanied by unconfirmed hot planet candidates. Therefore, superflares are possibly caused by stellar magnetic activities instead of planet-star interactions. We also find an extraordinary star TIC43472154, which exhibits about 200 superflares per year. In addition, the correlation between energy and duration of superflares ($T_{\\text {duration }} \\propto E^{\\beta}$) is analyzed. We derive the power-law index to be $\\beta=0.42\\pm0.01$, which is a little larger than $\\beta=1/3$ from the prediction according to magnetic reconnection theory.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2019-12-25T01:42:50.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "solar-type stars",
      "observation",
      "higher superflare frequency distribution",
      "robust superflare occurrence frequency",
      "little larger"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}