By Peter Cattermole PhD, FRAS (auth.)

As I write this brief preface, the purple orb of Mars is excessive within the jap sky, and is brighter than it's been for a few years. final evening my telescope back printed the unusual polar hood that's a characteristic of the planet at the moment in its cycle. as a result of its present prominence within the evening sky, it's a very acceptable time to assemble and reappraise what we all know of Mars and look ahead to the following wave of planetary exploration. The preliminary idea of writing a booklet approximately Mars is an exhilarating one; the practicalities all for operating via and finishing the undertaking are, even if, greater than a trifle exacting. the 1st challenge I encountered was once the sheer vastness of the library of data approximately Mars which now exists. the second one was once the common extension of the 1st, that's, how top to examine it and achieve extensively appropriate interpretations. i've got attempted to put in writing the tale of Mars in a logical and impartial manner, notwithstanding, all of us have our person prejudices, and that i will be lower than honest if i didn't admit to private bias the following and there. With this in brain, I apologise to any authors who may possibly suppose both misinterpreted or below properly said. The venture is now accomplished and has been beautifully ready via Chapman & Hall.

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99°W. many areas of smoother, less densely cratered plains between the large impact craters. The relative proportion of these intercrater plains compared to that of the more rugged cratered units varies from region to region. As has been mentioned, many of the intercrater surfaces are cut by short channel networks; others are ridged. Sometimes ridges may be seen crossing the intercrater plains and continuing along the same strike, inside large impact craters. 9 X 107 km2, of which about 36% is ridged.

90 Q' e..... 240 Solar declination (l) ..... 27 :::J cri 220 Q; a. E 2 (l) () CCI 't :::J (f) 160 60° 140 120 0 2 4 6 8 10 12 14 16 18 20 22 24 Time (hours) 300~--------------------------------~--~-------. 31 260 Q' e..... 240 ~ :::J T§(l) 220 a. E 2 (l) 200 ~ 't :::J (f) 140 120~ Fig. 13 Diurnal temperature variation as a function of latitude (after Michaux and Newburn, 1972). o ______________~__~____________~__~__~__~__~ 2 4 6 8 10 12 14 16 18 20 22 24 Local ti me (hou rs) The stratigraphy of Mars after, temperatures fell rapidly during the afternoon, this fall slowing down during the night and reaching the predawn minimum (Fig.

M. 2 ATMOSPHERIC PRESSURE VARIATIONS The abundances of minor constituents, like H 2 0, O 2 and 0 3 , vary with the season and also the geographical location; the total surface pressure also varies with the season. The latter was measured at both Viking lander sites, where a long enough run of data was obtained to show that during southern winter there was a gradual decrease in the surface atmospheric pressure which was then reversed as spring approached (Fig. 1). 4mbar and 10mbar, the higher values here probably reflecting the somewhat lower elevation of this site.

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