Upper Ionosphere of Mars During Solar Quiet and Disturbed Conditions - Planetary Exploration and Science: Recent Results and Advances - page 123

Fig. 7.6 ( a ) Electron density profiles on Mars obtained for 15 April and 26 April 2001. Two
profiles in red at 14:15 and 13:16 UT show significant enhancement at low altitude because of
solar flares which peaked in X-ray fluxes at Earth at 13:50 and 13:10 UT, respectively. On 15 April
there were five MGS profiles before the flare at 2:28, 6:23, 8:21, 10:19 and 12:17 UT and none
after the flare. On 26 April pre-flare profiles were available at 9:20 and 11:18 UT and post-flare
at 17:11 and 19:09 UT. ( b ) % differences between the flare affected profiles and the averages of
the other profiles on each day. The shading gives 1-¢ standard error in relative change in electron
density ( N e ) (Reprinted from Haider and Mahajan ( 2014 ) with kind permission from Springer)
the major characteristics and magnitudes of the measured solar X-ray spectra by
model calculation. Figure 7.7a, c, e present the calculated and measured solar X-ray
flux distribution from 29 May to 3 June 2003, 15 to 20 January 2005 and 12 to
18 May 2005, respectively, in the wavelength range 1-8 Å. Figure 7.7b, d, f show