Ionospheric Sensitivity to Different Representations of EUV Spectra

Details Ionospheric Sensitivity to Different Representations of EUV Spectra Ionospheric Sensitivity to Different Representations of EUV Spectra

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21b..05s&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH21B-05

Physics

2443 Midlatitude Ionosphere, 2479 Solar Radiation And Cosmic Ray Effects, 7538 Solar Irradiance

Scientific paper

It is well established that solar EUV radiation is responsible for the formation of the ionosphere, and in lieu of continuous direct observations, there exist a number of different models of this spectra. Empirical models have been developed from parameterized fits of past rocket and satellite measurements, while the newly developed NRLEUV model computes the spectra by accounting for the fractional coverage of solar magnetic features (active regions, network, coronal holes) and their temperature-dependent emissions. For a given level of solar activity, as determined by proxies (e.g. F10.7, Mg index), these models often produce considerably different spectra, but it remains to be seen how strongly these differences propagate through to ionospheric quantities such as the peak electron density (NmF2). In this work, we compare electron density profiles computed with the Time-Dependent Ionospheric Model (TDIM), using five different EUV representations as input. We see up to a factor of two spread in the modeled NmF2 during solar maximum decreasing to roughly 1.5 during solar minimum. Considerable differences are also seen in the peak density and profile shape of the E-layer. These results indicate that attempts to operationally specify and forecast the ionosphere will be limited until knowledge of the EUV spectral irradiance is better constrained, by regular observations and/or improved models.

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