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SOLAR DYNAMICS The coronas of stars transform the kinetic energy of solar electric currents into photons, radiated outward as starlight and radiating the ferrite surface of the core below the mantle where photons transform into electron positron pairs and electrons transform into field lines resulting in residual positrons which merge in trios, trios are trapped by transiting electrons and transform into protons. At high photon energy, electron positron pair production is the dominant mode of photon interaction with matter. First observed in Patrick Blackett’s cloud chamber, leading to the 1948 Nobel Prize in Physics. If the photon is near an atomic nucleus, the energy of a photon can be converted into an electron–positron pair: The Solid Solar Surface Model is based upon observations from the YOHKOH, SOHO and TRACE satellite programs, from spectral analysis data compiled by the SERTS program. This “running Difference” image of the surface was captured by SOHO. This image was taken on May 27th 2005 at 19:13 using the 195A filter that is sensitive to iron ion emissions. Photon transformation into protons cools the core and protons de-ionized with electrons into liquid metallic hydrogen, composing the solar mantle. The mantle is cooled at the surface, by evaporative cooling as liquid hydrogen sublimates into the solar winds of stars and interstellar medium of ionized plasma gas, which which escapes from sunspots and coronal holes.
Temperatures in the corona are upwards of 2 million degrees Fahrenheeit, while just 1,000 miles below, the underlying surface simmers at a balmy 10,000 F. How the Sun manages this feat remains one of the greatest unanswered questions in astrophysics; scientists call it the coronal heating problem. Solar cores are rotating arrays of equal radius, ionized spheres, draped in ferrite boundary layers, which transforms the momentum of moving charges into dipole moments which is captured by the field and increases the momentum of orbiting ions in the direction of core rotation, powering super rotation of the solar atmosphere and expanding heliosphere sheet, of solar ions.
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