Nucleifusion

Nucleifusion is the process by which light atomic nuclei combine to form a heavier nucleus, releasing energy in the process. In stars, thermonuclear fusion powers energy production under extreme temperatures and pressures. On Earth, achieving controlled nucleifusion requires heating fuel to very high temperatures and confining it long enough for fusion reactions to occur. The most studied reactions involve hydrogen isotopes, such as deuterium and tritium, which are favored for their relatively high reaction rates and energy per event.

The primary energy-releasing reactions are deuterium-tritium fusion, which yields a helium nucleus and a fast neutron, and alternative reactions such as deuterium-deuterium or proton-boron fusion. The energy output arises from a small mass difference between the reactants and products, converted to kinetic energy of the reaction products or captured as usable power.

Two main approaches have guided fusion research: magnetic confinement fusion (MCF) and inertial confinement fusion (ICF). MCF uses magnetic fields to confine a hot plasma for a period sufficient to sustain fusion, with devices such as tokamaks and stellarators. ICF aims to compress and heat small fuel capsules with intense laser or particle beams on nanosecond timescales to induce a brief, high-density fusion burst.

Key challenges include achieving net energy gain, maintaining plasma stability and confinement, managing heat loads on reactor surfaces, and developing materials and fuel cycles that can withstand extreme conditions. Economic viability and the supply of fuels like tritium also influence progress.

Current status, as of the early 2020s, shows substantial experimental advances but no sustained, commercially viable fusion power plant. Research facilities worldwide continue to explore confinement methods, fuel cycles, and reactor concepts, with the aim of delivering a safe, low-carbon energy source if technical hurdles can be overcome.