242 J, R. Mayer on Celestial Dynamics. 
Since gravity is 28 times greater on the sun’s surface than 
it is on our earth, a column of air on the former aa cause @ 
pressure 28 times greater than it would on our 1s 
great pressure compresses air as much as a pester of 8000° 
would expand it. 
In a still greater degree than this increased gravity do the 
qualities iin to gases affect the height of the solar atmo- 
atmosphere rapidly diminishes as we ascend, and increases as we 
descend. Generally speaking, rarefaction increases in a geome- 
trical ti Aen ihe the heights are in an arithmetical pro- 
. gression. If we ascend or descend 21, 5, or 30 miles, we find 
our Readéphiaie 10, 0,100, or a billion times more rarefied or more 
so rapidly with the "teeig as the latter joan If we assume 
08 increase and decrease on the sun to be ten times slower than 
tis on our earth, it follows that at the heights of 25, 50, and 
300 miles, a Farehaatiod of 10, 100, and a billion times respect 
ively, would be observed. The solar atmosphere, therefore, 
stor! ne attain a height of 400 geographical miles, or it cannot 
uch as ;},th of the sun’s radius. For if we take the 
density of the lowest strata of the sun’s atmosphere to be 1000 
times greater than that of our own near the level of the sea, 4 
density greater than that of water, and necessarily too bel 
then at a height of 400 miles this atmosphere would be 1 
billion times less dense than the earth’s paras that is : 
say, nd human Dediees ererasrees% it has ce 
here 
s, when free fry any solid particles, a deli 
at the a peat let 
ee :dinsurbances od the iar sais gees guia by most 
‘epson ad and party to be # cansed by 
the direct Jnfinence of = 
