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Energetics and timing of the hard and soft x-ray emissions in white light flares

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Abstract

By comparing the light curves in optical, hard x-ray, and soft x-ray wavelengths for 8 well-observed flares, we confirm previous results indicating that the white light flare (WLF) is associated with the flare impulsive phase. The WLF emission peaks within secondsafter the associated hard x-ray peak, and nearly two minutesbefore the 1–8 Å soft x-ray peak. It is further shown that the peak power in nonthermal electrons above 50 keV is typically an order of magnitudelarger, and the power in 1–8 Å soft x-rays radiated over 2π strdn at the time of the WLF peak is an order of magnitudesmaller, than the peak WLF power.

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Authors and Affiliations

  1. Phillips Laboratory (AFMC), Geophysics Directorate, National Solar Observatory/Sacramento Peak National Optical Astronomy Observatories, 88349, Sunspot, NM, USA

    Donald F. Neidig

  2. Space Sciences Laboratory, University of California, Berkeley, 94720, Berkeley, CA, USA

    Sharad R. Kane

Authors
  1. Donald F. Neidig
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  2. Sharad R. Kane
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Additional information

Operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. Partial support for the National Solar Observation is provided by the USAF under a Memorandum of Undestanding with the NSF.

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Neidig, D.F., Kane, S.R. Energetics and timing of the hard and soft x-ray emissions in white light flares. Sol Phys 143, 201–204 (1993). https://doi.org/10.1007/BF00619106

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  • DOI: https://doi.org/10.1007/BF00619106

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