Galactal and intersellar fields are a mild spectral decomposition, just enough to provide measurement coverage and separation of large clusters. Their Null points, matter, would hardly be noticeable to us. There wavelengths large, their quantization very fine.Later on, when the compaction nears completion, watching these field get violent and angry will a sight.
As phase around stars expands out, their granularity is limited by the the rate at which their centers of compaction can generate phase imbalance, having already begin field formation. But these gravity waves meet, they do not quite match, the vacuum gets simultaneous, and their granulartiy is is stabilized in successive waves. When this happens, even finer resolution phase imbalance is emitted at the inter stellar level. Pauli is maintained.
Looking at the article at the bottom of this post. Scientists working the same problem have found dust rings out side of young star regions. The outer part of the rings are where the stellar field meets, the inner part are when the gravitation meet. As the dust particles get compact, the gravitation and stellar reach Pauli equilibrium.
That, then matches much better the field length of gravity and magnetic. But my estimated field length of the electron is still too small, there is some charge energy I am missing. But mainly that is likely my lack of knowledge of atomic quantum numbers, and energy conservation at that level. I am looking for a way to get around that. This theory is real, it is working.
Stardust grains (also called presolar grains by meteoriticists) are contained within meteorites, from which they are extracted in terrestrial laboratories. The meteorites have stored those stardust grains ever since the meteorites first assembled within the planetary accretion disk more than four billion years ago. So-called carbonaceous chondrites are especially fertile reservoirs of stardust. Each stardust grain existed before the Earth was formed. Stardust is a scientific term referring to refractory dust grains that condensed from cooling ejected gases from individual presolar stars and mixed into the cloud from which the Solar System condensed.
Many different types of stardust have been identified by laboratory measurements of the highly unusual isotopic composition of the chemical elements that comprise each stardust grain. These refractory mineral grains may earlier have been coated with volatile compounds, but those are lost in the dissolving of meteorite matter in acids, leaving only insoluble refractory minerals. Finding the grain cores without dissolving most of the meteorite has been possible, but difficult and labor intensive (see presolar grains).
These scientists are working the same problem:
Astronomers using the new Atacama Large Millimeter/submillimeter Array (ALMA) have imaged a region around a young star where dust particles can grow by clumping together. This is the first time that such a "dust trap" has been clearly observed and modelled. It solves a long-standing mystery how dust particles in discs grow to larger sizes so that they can eventually form comets, planets, and other rocky bodies. The results are published in the journal Science on 7 June 2013. Astronomers now know that planets around other stars are plentiful. But they do not fully understand how they form and there are many aspects of planet (and comet and asteroid) formation that remain a mystery. However, new observations exploiting the power of ALMA are now answering one of the biggest questions: how do tiny grains of dust in the disc around a young star grow bigger and bigger — to eventually become rubble, and even boulders well beyond a meter in size? Computer models suggest that dust grains grow when they collide and stick together. However, when these bigger grains collide again at high speed they are often smashed to pieces and sent back to square one. Even when this does not happen, the models show that the larger grains would quickly move inwards because of friction between dust and gas and fall onto their parent star before they have a chance to grow even further. Somehow the dust needs a safe haven where the particles can continue growing until they are big enough to survive on their own [1]. To get past this vexing size limit, astronomers have theorized that swirling eddies in the disk could create dust traps, regions that enable dust particles to cling together, eventually setting the stage for the formation of larger and larger objects. But there was no observational proof of their existence up to now.
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