By Hans R. Pruppacher (auth.), S. I. Rasool (eds.)
About 3 years in the past Catherine de Berg and that i released a quick article in Nature during which we tried to give an explanation for why the chemistry of the ambience of the Earth is this day so different from that of our neighbor ing planets, Mars and Venus. Our surroundings consists in general of N2 and O with lines of A, H0, CO , zero , and so forth. , whereas the atmospheres of either 2 2 2 three Mars and Venus are nearly fullyyt made from CO , additionally, the Earth appears to be like 2 to be the one one ofthe 3 planets which has oceans ofliquid water at the floor. because the presence of liquid water on the earth is perhaps a vital requirement for all times to have originated and developed to its current nation, the query of the plain absence ofliquid water on Mars and Venus unexpectedly acquires major proportions. In our paper in Nature, and later in a extra distinctive dialogue of the topic (Planetary Atmospheres, in Exobiology, edited via C. Ponnamperuma, North Holland Publishing Co. ), we attempted to explain why we think that during the early background of the sun approach the entire terrestrial planets misplaced the atmospheres of H2 and He which they'd bought from the sun nebula on the time in their formation. those planets, thoroughly without atmos pheres, just like the Moon this present day, began gathering new gases that have been exhumed from the internal through the graduation of volcanic activity.
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2), given by K = C~ w(ulVnkT)1/2, where the surface area of a critical embryo on the water-insoluble substrate is approximately given by Q g ~ nrg 2, C~ is the number of single water vapor molecules adsorbed per unit surface area of the nucleating surface, and w is the rate of impact of water molecules from the vapor per unit surface area. Near ooe, the kinetic factor K varies between 1024 and 1027 depending on the particle's effectiveness for adsorbing water vapor. The prefactor of the exponent can approximately be taken to be 10254nrN2 .
121]. 121] are based on a thermodynamic and dynamic model which includes entrainment. In Fig. 15 the effect of the initial size spectrum of the dry, hygroscopic nuclei on the drop size spectrum is clearly reflected in the different times needed for aerosol particles in equilibrium with 99 % relative humidity (assumed to be the level of visible cloud) at time t = 0 to grow to drops of 20 and 30,um radius. After a time of about 7 min, 80 drops liter-I with radii larger than 20,um and 6 drops liter- I with radii larger than 30,um were present in a cloud which originated on an aerosol with the dry particle size distribution given in Fig.
6, where Sc is plotted as a function of rN for e = 5°, 7°, and 12° and where comparison is also made with the case e = 0° evaluated from Eq. (27). The results show that Sc strongly depends on the wetting angle of a particle as pointed out by McDonald . 2 x 10 - 5 cm. Insoluble particles with wetting angles larger than about 7° will not get involved at all in the condensation process no matter what their size is if it is assumed that 1 % supersaturation is a typical upper limit in atmospheric clouds.