Journal of Fusion Energy

, Volume 21, Issue 3, pp 193-198

First online:

Superfluidity in the Solar Interior: Implications for Solar Eruptions and Climate

  • Oliver K. ManuelAffiliated withUniversity of Missouri
  • , Barry W. NinhamAffiliated withUniversities of Florence and CagliariAustralian National University
  • , Stig E. FribergAffiliated withClarkson University

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Efforts to understand unusual weather or abrupt changes in climate have been plagued by deficiencies of the standard solar model (SSM) [1]. Although it assumes that our primary source of energy began as a homogeneous ball of hydrogen (H) with a steady, well-behaved H-fusion reactor at its core, observations instead reveal a very heterogeneous, dynamic Sun. As examples, the upward acceleration and departure of H+ ions from the surface of the quiet Sun and abrupt climatic changes, including geomagnetic reversals and periodic magnetic storms that eject material from the solar surface are not explained by the SSM. The present magnetic fields are probably deep-seated remnants of very ancient origin. These could have been generated from two mechanisms. These are (1) Bose-Einstein condensation [2] of iron-rich, zero-spin material into a rotating, superfluid, superconductor surrounding the solar core and/or (2) superfluidity and quantized vortices in nucleon-paired Fermions at the core [3].

Climate solar magnetic fields solar cycle Bose-Einstein condensates