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To show that if the hypothesis of foggy masses of solid, thenthe Genesis of the Solar system presents a visual proof of thislaw, for example, that the substance from which the Sun and planets,was once in a diffused form and that due to the gravity of atomsthere was a gradual concentration. According to this hypothesis, the Solar system, withthe origin of the part, there was the medium of space which wasunlimited and which was almost homogeneous in density, temperature andthe other physical properties. The difference of density and temperature of the inner andthe outer parts of the mass were the first impetus to the consolidation of mass. At the sametime inside the mass originated rotational motion, the speed of whichchanged in proportion to the distance from the center. These differentiations increased inthe number and extent until, until he developed the famous us organizedgroup of Sun, planets, and satellites, a group that represents numerousdifferences in the structure and actions of their members. So, between the Sunand planets there is a huge difference in volume and weight; there are minorthe difference of one from another planet or planets from satellites. There is also aa sharp distinction between the Sun - body, almost motionless (relative to theplanets of the Solar system) and planets orbiting it with a largespeed, and a minor difference in the speed and the periods of rotation of differentplanets in single and double perturbations of the satellites, moving in one and thethe same time naputstvuya around their body and around the Sun. Next,there is a big difference between the Sun and planets in relation totemperature; and there is reason to assume that the planets and their satellitesdiffer from each other in the degree of their warmth, and that whichthey receive from the Sun. In addition to all of the differentdifferences, we will take in consideration that planets and moons differ inthe mutual distances between them, and distances from the main body, the inclination of their orbits and axis, time of rotation around the axis, in the proportionand in the physical structure - we will see what a high degree of heterogeneityis the Solar system compared with the almost completelymisty homogeneous mass, from which, as suggested, did thissystem.
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