Modeling of the ionospheric response to the solar eclipse of 24 October 1995

In this paper the ionospheric effects of the solar eclipse of October 24, 1 995 were investigated using a two-dimensional ionospheric theoretical model In the calculations, only the depression of solar EUV fluxes during the co urse of the eclipse was taken into account under the solar eclipse conditio n, (1) During the period of the eclipse, the optical effects were quite cle ar at the lower altitudes of the ionosphere, while the responses to the ecl ipse were weaker, delayed, but longer in duration at the higher altitudes. (2) The lower the magnetic latitude, the stronger was the response to the s olar eclipse, In low latitude regions, the values of f(0)F(2) on the eclips e day were lower compared with those under the control conditions, whereas h(m)F(2) values were higher. (3) Near the magnetic equator there was a shar p transition in h(m)F(2) after the maximum phase of obscuration, and a sola r F-1.5 layer appeared below the normal peak height of the F-2 layer. (4) A fter the maximum phase, the effects of the eclipse lasted longer near Haina n, and a secondary depression occurred over the magnetic equator. The mecha nisms that may bet responsible for the eclipse-caused effects are discussed here.