A superconductor of paired protons is thought to form in the core of neutron stars soon after their birth. Minimum energy conditions suggest magnetic flux is expelled from the superconducting region due to the Meissner effect, such that the neutron star core is largely devoid of magnetic fields for some nuclear equation of state and proton pairing models. We show via neutron star cooling simulations that the superconducting region expands faster than flux is expected to be expelled because cooling timescales are much shorter than timescales of magnetic field diffusion. Thus magnetic fields remain in the bulk of the neutron star core for at least 10^6-10^7 yr. We estimate the size of flux free regions at 10^7 yr to be <~ 100 m for a magnetic field of 10^11 G and possibly smaller for stronger field strengths. For proton pairing models that are narrow, magnetic flux may be completely expelled from a thin shell of approximately the above size after 10^5 yr. This shell may insulate lower conductivity outer layers, where magnetic fields can diffuse and decay faster, from fields maintained in the highly conducting deep core.
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机译:用等离子体约束实现重力场的动态控制热核聚变(TLTS)方法,通过热辐射等离子体绝缘的壁反应堆防止中子辐射并节省磁场和等离子体的混合,使用旋转磁场的异步磁惯性约束反应堆(AMITYAR和HFM)为实施该方法,在该反应器中点燃热核反应的方法,爆炸式等离子发生器(VIP)的实施方法,以及具有HFM的特立普安瓿,以实现D + T反应和具有超高温热度的HFM D +3НЕ和1Н+11В的高温反应