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XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models
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  • Open Access
  • Published: 30 May 2008

XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models

  • Thomas N. Woods1,
  • Phillip C. Chamberlin1,
  • W. K. Peterson1,
  • R. R. Meier2,
  • Phil G. Richards2,
  • Douglas J. Strickland3,
  • Gang Lu4,
  • Liying Qian4,
  • Stanley C. Solomon4,
  • B. A. Iijima5,
  • A. J. Mannucci5 &
  • …
  • B. T. Tsurutani5 

Solar Physics volume 250, pages 235–267 (2008)Cite this article

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  • 57 Citations

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Abstract

Solar soft X-ray (XUV) radiation is highly variable on all time scales and strongly affects Earth’s ionosphere and upper atmosphere; consequently, the solar XUV irradiance is important for atmospheric studies and for space weather applications. Although there have been several recent measurements of the solar XUV irradiance, detailed understanding of the solar XUV irradiance, especially its variability during flares, has been hampered by the broad bands measured in the XUV range. In particular, the simple conversion of the XUV photometer signal into irradiance, in which a static solar spectrum is assumed, overestimates the flare variations by more than a factor of two as compared to the atmospheric response to the flares. To address this deficiency in the simple conversion, an improved algorithm using CHIANTI spectral models has been developed to process the XUV Photometer System (XPS) measurements with its broadband photometers. Model spectra representative of quiet Sun, active region, and flares are combined to match the signals from the XPS and produce spectra from 0.1 to 40 nm in 0.1-nm intervals for the XPS Level 4 data product. The two XPS instruments are aboard NASA’s Solar Radiation and Climate Experiment (SORCE) and Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) satellites. In addition, the XPS responsivities have been updated for the latest XPS data processing version. The new XPS results are consistent with daily variations from the previous simple conversion technique used for XPS and are also consistent with spectral measurements made at wavelengths longer than 27 nm. Most importantly, the XPS flare variations are reduced by factors of 2 – 4 at wavelengths shorter than 14 nm and are more consistent, for the first time, with atmospheric response to solar flares. Along with the details of the new XPS algorithm, several comparisons to dayglow and photoelectron measurements and model results are also presented to help verify the accuracy of the new XUV irradiance spectra.

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Authors and Affiliations

  1. Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO, 80303, USA

    Thomas N. Woods, Phillip C. Chamberlin & W. K. Peterson

  2. Physics and Astronomy Department, George Mason University, Fairfax, VA, 22030, USA

    R. R. Meier & Phil G. Richards

  3. Computational Physics, Inc., Springfield, VA, 22151, USA

    Douglas J. Strickland

  4. High Altitude Observatory, National Center for Atmospheric Research, Boulder, CO, 80309, USA

    Gang Lu, Liying Qian & Stanley C. Solomon

  5. Jet Propulsion Laboratory, Pasadena, CA, 91109, USA

    B. A. Iijima, A. J. Mannucci & B. T. Tsurutani

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  1. Thomas N. Woods
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Correspondence to Thomas N. Woods.

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Open Access This is an open access article distributed under the terms of the Creative Commons Attribution Noncommercial License (https://creativecommons.org/licenses/by-nc/2.0), which permits any noncommercial use, distribution, and reproduction in any medium, provided the original author(s) and source are credited.

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Woods, T.N., Chamberlin, P.C., Peterson, W.K. et al. XUV Photometer System (XPS): Improved Solar Irradiance Algorithm Using CHIANTI Spectral Models. Sol Phys 250, 235–267 (2008). https://doi.org/10.1007/s11207-008-9196-6

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  • Received: 26 December 2007

  • Accepted: 22 April 2008

  • Published: 30 May 2008

  • Issue Date: August 2008

  • DOI: https://doi.org/10.1007/s11207-008-9196-6

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Keywords

  • Solar Cycle
  • Total Electron Content
  • Solar Irradiance
  • Solar Cycle Variation
  • Extreme Ultraviolet Variability Experiment
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