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02 Stellar Evolution

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Submitted by LoneBear on Thu, 03/27/2014 - 13:45

Modern astronomy differs from Reciprocal Astronomy in one major aspect: the stellar combustion process. An important aspect, for it is the combustion process that determines the stellar evolutionary sequence.

Figure 2: Modern Astronomy Stellar Evolution

Modern astronomy relies on the fusion of hydrogen to helium, the process observed within the photosphere (the outer layers of a star). This process starts out with a bang—a supernova—which forms a blue giant star, that gradually cools down, moves down the Main Sequence, and burns out due to lack of hydrogen fuel. At the end of its life cycle, a number of strange things occur, such as its sudden bloating up to a red giant, then re-condensing down to a white dwarf, or altogether vanishing from the universe in a “black hole.”

Reciprocal System astronomy is a bit more straight-forward, analogous to heating up a piece of metal. The only thing required to build a star is “matter” (dust and rock) and simple gravitation does the rest.


Figure 3: Reciprocal System Stellar Evolution

Stars, in the Reciprocal System, start out as large clouds of dust emitting infrared light from the sparse collisions of atoms. The gas and dust are pulled together by gravitation, and collisions become more frequent, heating the aggregate up so it glows dull red—a red super-giant. As more matter is pulled in, the gravitational pull of the star increases, reducing its size and increasing its temperature, moving down through orange giant stars, and on to the Main Sequence. From this point, the stellar matter can no longer be compressed, so the star becomes physically larger, and moves up the Main Sequence towards the blue giant—exactly the opposite evolutionary path as modern astronomy.

The most important aspect of the stellar evolutionary system that we are considering is the death of a star—the supernova. In the Reciprocal System, it comes in two varieties, both of which are observed by modern astronomers. The first occurs when the star reaches its thermal limit, and explodes as a “Type I” supernova. This only happens to the blue giant O-class stars, for only they are hot enough to reach the thermal limit.

The second stellar death can happen to any class star—the age limit. When the matter composing the star reaches a certain age (determined by isotopic mass), it explodes. When a large enough chunk of matter does this at the same time, a “Type II” supernova forms. The Type II supernova is more violent than the Type I, and typically propels matter into the ultra-high speed range (designated 3-x), moving far in excess of the speed of light.

The supernova explosion throws the outer layers of the sun off into space, comprised mostly of gases and light elements. The explosion also forces an implosion of the heavy elements in the core. (A spatial “implosion” in the Reciprocal system is a temporal explosion—the imploding matter expands in time, and contracts in space.)

As mentioned, stars are created from simple aggregates of dust and rock in space, so the obvious result of a supernova is a large cloud of expanding matter, which will eventually slow, stop, and re-condense to form another star at the center of gravity of the debris field, usually quite near where the original supernova occurred.

The second supernova byproduct—the imploded stellar core—forms a white dwarf star, with all of its unusual characteristics: inverse density gradient, intense magnetic field, quantized emission, and all the phenomenon associated with intermediate-speed (2-x) motion.1

The supernova can be considered a “birthing process” of either a binary star system (red giant/white dwarf pair), or a single star with a planetary system, depending on its generation. (A “generation” being the number of times a star has been through the supernova/reformed star phase.)