Re-Estimation of Solar Corona Coefficients (a, B, c) by Using MGS & Mex Spacecraft Datas

Details Re-Estimation of Solar Corona Coefficients (a, B, c) by Using MGS & Mex Spacecraft Datas Re-Estimation of Solar Corona Coefficients (a, B, c) by Using MGS & Mex Spacecraft Datas

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1828v&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1828

Physics

Scientific paper

The Sun is one of the most studied star in the universe. It has many puzzling features and one of them is solar corona. The solar corona are the result of high density and strongly turbulent ionized gases (Plasma) being ejected from the Sun. During superior solar conjunction, the line of sight between the Earth and a spacecraft passes near the sun. When radio frequency waves pass through these regions, the signals suffer severe degradation or perturbed by the solar corona. The purpose of this study is to reduce the effect of solar corona on the range data when the signal raypath passes through the solar corona and then to estimate new solar corona coefficients. The model (Eq. 1) used for estimation of solar corona effect (during round-trip of propagation time) has been taken from Anderson (2002) or Moyer (2000).

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