Helium accreting slowly onto the surface of a neutron star accumulates in a thin surface layer. After reaching a depth of approximately 100 m and a density of about 2 x 10(8) gm cm(-3), the helium layer becomes unstable and a thermonuclear runaway initiates at its base. Since the runaway time scale is much shorter than the accretion time scale, it is likely that ignition will occur at a single point instead of simultaneously over the entire surface. This conclusion is supported by observations of brightness oscillations in X-ray bursts. In this case, a burning front will propagate across the surface, eventually consuming the entire layer. This paper describes high-resolution two-dimensional simulations of the propagation of a helium detonation across the surface of a neutron star. [References: 12]
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机译：缓慢吸收到中子星表面上的氦气堆积在薄的表层中。到达约100 m的深度和约2 x 10（8）gm cm（-3）的密度后，氦气层变得不稳定，并且在其底部开始出现热核逸散。由于失控时间尺度比积聚时间尺度短得多，因此点火很可能在单个点发生，而不是在整个表面上同时发生。该结论得到X射线猝发亮度振荡观察的支持。在这种情况下，燃烧的前沿将在整个表面上传播，最终消耗整个层。本文描述了氦爆轰在中子星表面传播的高分辨率二维模拟。 [参考：12]
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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
