Resumen de La ingeniería nuclear y el desarrollo de mecanismos de fusión por confinamiento magnético
- español
La fusión nuclear es el proceso mediante el cual los núcleos ligeros se unen para formar núcleos más pesados, y es el proceso que genera la energía del sol y de las estrellas (estas reacciones de fusión se producen a temperaturas del orden de los 150 millones de grados Celsius). El reto de la fusión es reproducir en la Tierra las reacciones que se producen en el interior de las estrellas para construir reactores capaces de satisfacer una parte sustancial de las necesidades energéticas del planeta a medio plazo.
- English
Nuclear fusion is the process by which light nuclei combine to form heavier nuclei, and is the process that generates energy from the sun and stars (these fusion reactions occur at temperatures of the order of 150 million Celsius). Densities of the order of 1020 m-3 and ion temperatures of about 10 keV are key features which ensure a stable state of ionization of matter called "plasma". The fusion process is one in experimentally accessible reactive deuterium and tritium nuclei generating an alpha particle and neutron. From the kinetic energy generated in the fusion of deuterium and tritium nuclei, 80% reside in neutral particles (neutrons) while 20% use in the nuclei of He (á particles). Visible spectroscopy, Thomson scattering, Interferometry microwave, Probes heavy ions, and Langmuir probes are some diagnostic systems used to characterize the material in this state. The challenge of the fusion is duplicated on Earth reactions occurring inside the star; therefore density in experimental nuclear fusion devices must be 15 orders of magnitude higher than the gas present in the interstellar and about 15 orders of magnitude lower than that found in the interior of some stars. These specifications should meet in a reactor capable of meeting a substantial portion of the world's energy needs in the short term.
Keywords: nuclear fusion, Stellerator, Tokamak,
