COREPHYSICS

• Protostellides are stellides that peakmassed as protostars.
• Protostellides peakmassed up to 0.8 solarmasses.
• Protostars form primarily by the accretion of nucleons and nuclides.
• Protostellides form by the collapse of accreted nucleons and nuclides.
• Protostellides are a monocore nucleus and teelosphere.
• Protostellides reactivate with sufficient further accretion.

• Protostars are understable protostellides.
• Protostar primary content is nucleons and nuclides.
• Protostars are a nucleus inside a teelosphere inside a gravitysheath inside a gravitysheath interface.
• Protostars have an atmosphere as conditions dictate.
• Protostars have an ocean as conditions dictate.
• Protostar nucleuses are liquidbonded as conditions dictate.
• Protostar nucleuses are liquidbonded and solidbonded as conditions dictate.
• Protostars peakmass up to 0.8 solarmasses.
• Protostars undergo nucleon and nuclide collapse during semistabilisation.
• Protostar collapses are gravitycollapse and emissioncollapse.

• Protostars semistabilise as protostellides.
• Semistabilisation is achieved by ejecting more gravitymassvelocity than is absorbed.
• Gravitymassvelocity ejection is by gravitycollapse and emissioncollapse.
• Gravitycollapse is protostar contraction by teelstream ejection.
• Emissioncollapse is nucleon and nuclide contraction by proton emission.
• Protostar nuclide stratify by isotopenumber as conditions permit.
• Protostar content stratifies by solidbonding, liquidbonding, and gasbonding as conditions permit.

• Objects with a peakmass too low for the fusion of subphotonics into isotopes.
• Grains -
• Objects with a peakmass too low to contract the nucleus to a spheroid.
• Planets -
• Spheroid objects with a peakmass between grains and giantplanets (jupiters).
• Giantplanets -
• Spheroid objects with a peakmass between planets and 0.8 of a solarmass.

• Nucleus
  • Protostar nuclei are isotopes and molecules.
  • With sufficient mass, protostar nuclei stratify.
  • Stratification is by increasing massdensity from surface to centre. 
  • Stratums are fractured by turbulence.
  • Teelstream systems flow through protostar nuclei.
  • Protostar nuclei of sufficient mass can have plasmastreams.
• Atmosphere
  • The complexity, density, and extent of protostar atmospheres increases with mass.
  • The complexity, density, and extent of protostar atmospheres alters by interaction with adjacent objects.
  • Protostar atmospheres are nucleons, isotopes and molecules.
  • Grain atmospheres are tenuous or nonexisting.
    
  • With increasing protostar mass, atmospheres stratify.
  • Stratification is by increasing massdensity from top to bottom.
  • Stratums are fractured by turbulence.
  • Teelstream systems flow through protostar atmospheres.
  • Protostar atmospheres of sufficient mass can have plasmastreams.
• Teelosphere
  • The complexity, density, and extent of protostar teelospheres increases with mass.
  • The complexity, density, and extent of protostar teelospheres alters by interaction with adjacent objects.
  • Teelospheres form into teelstream systems.
  • Teelstream systems in lower-mass protostars are centrifugal or chaotic.
  • Teelstream systems in higher mass protostars axial overall with regional centrifugalities.

• Protostars form and grow by accretion.
• Accretion adds energy and mass to a protostar.
• Per the energy/mass differential, accretion adds more energy than mass.
• Thus, accreting protostars are understable.
• Thus accreting protostars are simultaneously undergoing accretion expansion and stabilisation contraction.
• Rule of thumb:
  • Before peakmass, accretion expansion dominates stabilisation contraction.
  • After peakmass, stabilisation contraction dominates accretion expansion.
• Protostars stabilise as cold protostars.
• Most protostars are accreted by more massive accretides before they can stabilise.

• Protostars stabilise by emission and ejection.
  • Emissions
    • Photons emitted by understable protons.
  • Ejections
    • Nonphotonic content ejected per energy/mass differential mechanism.
• Protostars can only stabilise after all accretion has ceased.
• Stable protostars are understabilised by further accretion.