We explore the conditions prevailing in primordial planets in the frameworkof the HGD cosmologies as discussed by Gibson and Schild. The initial stages ofcondensation of planet-mass H-4He gas clouds in trillion-planet clumps is setat 300,000 yr (0.3My) following the onset of plasma instabilities when ambienttemperatures were >1000K. Eventual collapse of the planet-cloud into a solidstructure takes place against the background of an expanding universe withdeclining ambient temperatures. Stars form from planet mergers within theclumps and die by supernovae on overeating of planets. For planets produced bystars, isothermal free fall collapse occurs initially via quasi equilibriumpolytropes until opacity sets in due to molecule and dust formation. Thecontracting cooling cloud is a venue for molecule formation and the sequentialcondensation of solid particles, starting from mineral grains at hightemperatures to ice particles at lower temperatures, water-ice becomesthermodynamically stable between 7 and 15 My after the initial onset ofcollapse, and contraction to form a solid icy core begins shortly thereafter.Primordial-clump-planets are separated by ~ 1000 AU, reflecting the highdensity of the universe at 30,000 yr. Exchanges of materials, organic moleculesand evolving templates readily occur, providing optimal conditions for aninitial origin of life in hot primordial gas planet water cores when adequatelyfertilized by stardust. The condensation of solid molecular hydrogen as anextended outer crust takes place much later in the collapse history of theprotoplanet. When the object has shrunk to several times the radius of Jupiter,the hydrogen partial pressure exceeds the saturation vapour pressure of solidhydrogen at the ambient temperature and condensation occurs.
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