{
  "id": "1004.4259",
  "version": "v1",
  "published": "2010-04-24T06:33:55.000Z",
  "updated": "2010-04-24T06:33:55.000Z",
  "title": "G-band and Hard X-ray Emissions of the 2006 December 14 flare observed by Hinode/SOT and RHESSI",
  "authors": [
    "Kyoko Watanabe",
    "Sam Krucker",
    "Hugh Hudson",
    "Toshifumi Shimizu",
    "Satoshi Masuda",
    "Kiyoshi Ichimoto"
  ],
  "comment": "15 pages, 7 figures, accepted for publication in ApJ",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "We report on G-band emission observed by the Solar Optical Telescope onboard the Hinode satellite in association with the X1.5-class flare on 2006 December 14. The G-band enhancements originate from the footpoints of flaring coronal magnetic loops, coinciding with non-thermal hard X-ray bremsstrahlung sources observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager. At the available 2 minute cadence, the G-band and hard X-ray intensities are furthermore well correlated in time. Assuming that the G-band enhancements are continuum emission from a blackbody, we derived the total radiative losses of the white-light flare (white-light power). If the G-band enhancements additionally have a contribution from lines, the derived values are overestimates. We compare the white-light power with the power in hard X-ray producing electrons using the thick target assumption. Independent of the cutoff energy of the accelerated electron spectrum, the white-light power and the power of accelerated electrons are roughly proportional. Using the observed upper limit of ~30 keV for the cutoff energy, the hard X-ray producing electrons provide at least a factor of 2 more power than needed to produce the white-light emission. For electrons above 40 keV, the powers roughly match for all four of the time intervals available during the impulsive phase. Hence, the flare-accelerated electrons contain enough energy to produce the white-light flare emissions. The observed correlation in time, space, and power strongly suggests that electron acceleration and white-light production in solar flares are closely related. However, the results also call attention to the inconsistency in apparent source heights of the hard X-ray (chromosphere) and white-light (upper photosphere) sources.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2010-04-24T06:33:55.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "hard x-ray emissions",
      "energy solar spectroscopic imager",
      "high energy solar spectroscopic",
      "ramaty high energy solar",
      "hard x-ray bremsstrahlung sources"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/715/1/651",
      "journal": "The Astrophysical Journal",
      "year": 2010,
      "month": "May",
      "volume": 715,
      "number": 1,
      "pages": 651
    },
    "note": {
      "typesetting": "TeX",
      "pages": 15,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 853055,
      "adsabs": "2010ApJ...715..651W"
    }
  }
}