@prefix dbo: .
@prefix dbr: .
dbr:Flying_saucer dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Cataclysmic_variable_star dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Tungsten dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:X-ray_binary dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Gamma_ray dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Astrophysics dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Astrophysical_X-ray_source dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Pre-main-sequence_star dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Super_soft_X-ray_source dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Theoretical_astronomy dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Crab_Nebula dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Bremsstrahlung dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Magnetic_reconnection dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Radiation dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Weak_interaction dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Ray_Kidder dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:List_of_Romanian_inventors_and_discoverers dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Timeline_of_stellar_astronomy dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Top_Gear_3000 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Black_hole_starship dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:SN_2011dh dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Ralf_Mackenbach dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Helium-3 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Helium-4 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Francium dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Chalcogen dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_isomer dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Michio_Kaku dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Strong_interaction dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Star_lifting dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Helmholtz_Association dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Institute_of_Applied_Physics_and_Computational_Mathematics dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Leonardo_Mascheroni dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Eric_Burhop dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Bruno_Pontecorvo dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Lewi_Tonks dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_power_in_Taiwan dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_safety_and_security dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:TAE_Technologies dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Ceramic_matrix_composite dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Theta_pinch dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Age_of_Earth dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Faint_young_Sun_paradox dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Psi_Persei dbo:wikiPageWikiLink dbr:Nuclear_fusion .
@prefix ns2: .
ns2:_A_Cassini_Space_Odyssey dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Ross_154 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Delta_Pavonis dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Ring_Nebula dbo:wikiPageWikiLink dbr:Nuclear_fusion .
@prefix ns3: .
ns3:_Hell_on_Earth dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Internal_heating dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Levitated_dipole dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:List_of_most_massive_stars dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Search_for_extraterrestrial_intelligence dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Science_and_technology_in_Spain dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Epsilon_Persei dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Gliese_758 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Gliese_777 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:NGC_4631 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:NGC_6397 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Theta_Cygni dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Mars_to_Stay dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Transhuman_Space dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:MOA-2007-BLG-192Lb dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Colonization_of_the_Solar_System dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Zeta_Ophiuchi dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Thuban dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Future_of_space_exploration dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:G-type_main-sequence_star dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Habitability_of_red_dwarf_systems dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:John_DeChancie dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:AP_Columbae dbo:wikiPageWikiLink dbr:Nuclear_fusion .
@prefix ns4: .
ns4:_Odyssey_Two dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Alpha_Pavonis dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Parasites_Lost dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Far_side_of_the_Moon dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:HD_28185 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:HR_3384 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:HR_8799 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Harrison_Schmitt dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Iota_Centauri dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Solar_neutrino dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Lambda_Aquilae dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Discovery_One dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Double_planet dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Planetary_mass dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Cities_in_Flight dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:IK_Pegasi dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Olduvai_theory dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Origin_and_occurrence_of_fluorine dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Exploration_of_Jupiter dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Planetary_civilization dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Plasma_beta dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Moving_Earth dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Self-replicating_machines_in_fiction dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Period_1_element dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_chemistry dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_engineering dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Triple-alpha_process dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Elastic_scattering dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Energy_amplifier dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_data dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Alexander_Andreevich_Samarskii dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Yuri_Oganessian dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Plasma-facing_material dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Timeline_of_quantum_mechanics dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Gammasphere dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Ouyang_Ziyuan dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Carbon-burning_process dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Isotopes_of_lithium dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Introduction_to_the_heaviest_elements dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Taylor_Wilson dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Kardashev_scale dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Superheavy_element dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Marshall_Holloway dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Institute_for_Theoretical_and_Experimental_Physics dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Impulse_generator dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Even_and_odd_atomic_nuclei dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Fission_barrier dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:S-factor dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Hitlers_Bombe dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:The_Case_for_Mars dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Iron_peak dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Heinrich_Hora dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Epsilon_Reticuli dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_explosion dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Mark_Hatfield dbo:wikiPageWikiLink dbr:Nuclear_fusion .
@prefix rdfs: .
dbr:ITER rdfs:seeAlso dbr:Nuclear_fusion ;
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Osaka_University dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Neutron_bomb dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Synthetic_element dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Einsteinium dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Unbiunium dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:List_of_plasma_physics_articles dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_pulse_propulsion dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Technology_transfer dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Formation_and_evolution_of_the_Solar_System dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Gas_giant dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Asymptotic_giant_branch dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Giant_planet dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Orion_Nebula dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nebular_hypothesis dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Protostar dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Stellar_nucleosynthesis dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Helium_flash dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Big_Bang_nucleosynthesis dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:T_Tauri_star dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Black_dwarf dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Bachelor_of_Engineering dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Project_Excalibur dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Nuclear_thermal_rocket dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Inertial_electrostatic_confinement dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Bruno_Rossi dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Polywell dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Plasma_Sources_Science_and_Technology dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:The_Seven_Storey_Mountain dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:LASNEX dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Epsilon_Scorpii dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Hidetsugu_Ikegami dbo:wikiPageWikiLink dbr:Nuclear_fusion .
@prefix foaf: .
@prefix wikipedia-en: .
wikipedia-en:Nuclear_fusion foaf:primaryTopic dbr:Nuclear_fusion .
dbr:WR_102 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Star dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:WR_142 dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:WR_93b dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:WR_30a dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Supernova dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbo:wikiPageWikiLink dbr:Nuclear_fusion .
dbr:Planetary_nebula dbo:wikiPageWikiLink dbr:Nuclear_fusion .
@prefix rdf: .
@prefix owl: .
dbr:Nuclear_fusion rdf:type owl:Thing ,
dbo:Disease ;
rdfs:label "Kernfusie"@nl ,
"\u6838\u805A\u53D8"@zh ,
"Fusion nucl\u00E9aire"@fr ,
"\u6838\u878D\u5408\u53CD\u5FDC"@ja ,
"\uD575\uC735\uD569"@ko ,
"Comhle\u00E1 n\u00FAicl\u00E9ach"@ga ,
"Nuclear fusion"@en ,
"Reakcja termoj\u0105drowa"@pl ,
"Kernfusion"@de ,
"\u0422\u0435\u0440\u043C\u043E\u044F\u0434\u0435\u0440\u043D\u0430\u044F \u0440\u0435\u0430\u043A\u0446\u0438\u044F"@ru ,
"Fusi\u00F3 nuclear"@ca ,
"Fusione nucleare"@it ,
"K\u00E4rnfusion"@sv ,
"Jadern\u00E1 f\u00FAze"@cs ,
"\u0627\u0646\u062F\u0645\u0627\u062C \u0646\u0648\u0648\u064A"@ar ,
"Fus\u00E3o nuclear"@pt ,
"\u03A0\u03C5\u03C1\u03B7\u03BD\u03B9\u03BA\u03AE \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7"@el ,
"Fusi nuklir"@in ,
"Fuzio"@eo ,
"Fusio nuklear"@eu ,
"Fusi\u00F3n nuclear"@es ,
"\u042F\u0434\u0435\u0440\u043D\u0438\u0439 \u0441\u0438\u043D\u0442\u0435\u0437"@uk ;
rdfs:comment "K\u00E4rnfusion \u00E4r den process d\u00E5 atomk\u00E4rnor sm\u00E4lter samman och bildar st\u00F6rre och tyngre k\u00E4rnor. P\u00E5 grund av de sm\u00E5 atomk\u00E4rnornas l\u00E5ga bindningsenergi per nukleon kan man \"tj\u00E4na\" (frig\u00F6ra) energi om man sl\u00E5r ihop tv\u00E5 sm\u00E5 k\u00E4rnor till en tyngre. I stj\u00E4rnor f\u00F6rekommer k\u00E4rnfusion i mitten av stj\u00E4rnan, och det \u00E4r detta som \u00E4r deras energik\u00E4lla. P\u00E5 jorden f\u00F6rekommer fusion i st\u00F6rre omfattning endast i v\u00E4tebomber, men mycket pengar och forskning har lagts ner p\u00E5 att kunna anv\u00E4nda fusion som praktisk anv\u00E4ndbar energik\u00E4lla, precis vad som har skett med fission (k\u00E4rnklyvning). F\u00F6r att fusion ska kunna ske m\u00E5ste f\u00F6rst extrema temperaturer och tryck uppn\u00E5s, vilket bland annat den planerade reaktorn ITER ska f\u00F6rs\u00F6ka \u00E5stadkomma. Att kunna genomf\u00F6ra fusion under mindre extrema f\u00F6rh\u00E5llanden och skala vore en u"@sv ,
"\u03A0\u03C5\u03C1\u03B7\u03BD\u03B9\u03BA\u03AE \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7 (\u03C3\u03C5\u03BD + \u03C4\u03AE\u03BE\u03B7) \u03BF\u03BD\u03BF\u03BC\u03AC\u03B6\u03B5\u03C4\u03B1\u03B9 \u03B7 \u03C3\u03C5\u03BD\u03AD\u03BD\u03C9\u03C3\u03B7 \u03B5\u03BB\u03B1\u03C6\u03C1\u03CE\u03BD \u03C0\u03C5\u03C1\u03AE\u03BD\u03C9\u03BD \u03C3\u03B5 \u03B2\u03B1\u03C1\u03CD\u03C4\u03B5\u03C1\u03BF\u03C5\u03C2 \u03BC\u03B5 \u03C4\u03B1\u03C5\u03C4\u03CC\u03C7\u03C1\u03BF\u03BD\u03B7 \u03B1\u03C0\u03B5\u03BB\u03B5\u03C5\u03B8\u03AD\u03C1\u03C9\u03C3\u03B7 \u03B5\u03BD\u03AD\u03C1\u03B3\u03B5\u03B9\u03B1\u03C2, \u03B4\u03B7\u03BB\u03B1\u03B4\u03AE \u03C0\u03C1\u03CC\u03BA\u03B5\u03B9\u03C4\u03B1\u03B9 \u03B3\u03B9\u03B1 \u03B5\u03BE\u03CE\u03B8\u03B5\u03C1\u03BC\u03B7 \u03B1\u03BD\u03C4\u03AF\u03B4\u03C1\u03B1\u03C3\u03B7. \u0392\u03AD\u03B2\u03B1\u03B9\u03B1 \u03B3\u03B9\u03B1 \u03BD\u03B1 \u03B8\u03B5\u03C9\u03C1\u03B7\u03B8\u03B5\u03AF \u03B5\u03BE\u03CE\u03B8\u03B5\u03C1\u03BC\u03B7 \u03B1\u03BD\u03B1\u03C6\u03B5\u03C1\u03CC\u03BC\u03B1\u03C3\u03C4\u03B5 \u03C3\u03B5 \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7 \u03B5\u03BB\u03B1\u03C6\u03C1\u03CE\u03BD \u03C0\u03C5\u03C1\u03AE\u03BD\u03C9\u03BD \u03BC\u03AD\u03C7\u03C1\u03B9 \u03C4\u03BF \u03C3\u03AF\u03B4\u03B7\u03C1\u03BF-56 \u03AE \u03BD\u03B9\u03BA\u03AD\u03BB\u03B9\u03BF-62. \u039A\u03B1\u03C4\u03AC \u03C4\u03B7 \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7 \u03B2\u03B1\u03C1\u03CD\u03C4\u03B5\u03C1\u03C9\u03BD \u03C0\u03C5\u03C1\u03AE\u03BD\u03C9\u03BD \u03B1\u03C0\u03CC \u03B1\u03C5\u03C4\u03BF\u03CD\u03C2 \u03C5\u03C0\u03AC\u03C1\u03C7\u03B5\u03B9 \u03B5\u03BD\u03B5\u03C1\u03B3\u03B5\u03B9\u03B1\u03BA\u03CC \u03AD\u03BB\u03BB\u03B5\u03B9\u03BC\u03BC\u03B1 \u03BA\u03B1\u03B9 \u03B7 \u03B1\u03BD\u03C4\u03AF\u03B4\u03C1\u03B1\u03C3\u03B7 \u03B3\u03AF\u03BD\u03B5\u03C4\u03B1\u03B9 \u03B5\u03BD\u03B4\u03CC\u03B8\u03B5\u03C1\u03BC\u03B7."@el ,
"\u042F\u0301\u0434\u0435\u0440\u043D\u0438\u0439 \u0441\u0438\u0301\u043D\u0442\u0435\u0437 \u2014 \u0446\u0435 \u043F\u0440\u043E\u0446\u0435\u0441, \u043F\u0456\u0434 \u0447\u0430\u0441 \u044F\u043A\u043E\u0433\u043E \u0434\u0432\u0430, \u0430\u0431\u043E \u0431\u0456\u043B\u044C\u0448\u0435, \u0430\u0442\u043E\u043C\u043D\u0456 \u044F\u0434\u0440\u0430 \u043E\u0431'\u0454\u0434\u043D\u0443\u044E\u0442\u044C\u0441\u044F, \u0444\u043E\u0440\u043C\u0443\u044E\u0447\u0438 \u0432\u0430\u0436\u0447\u0435 \u044F\u0434\u0440\u043E. \u0414\u043B\u044F \u0437\u0431\u043B\u0438\u0436\u0435\u043D\u043D\u044F \u0430\u0442\u043E\u043C\u043D\u0438\u0445 \u044F\u0434\u0435\u0440 \u0434\u043E\u0441\u0442\u0430\u0442\u043D\u044C\u043E \u0442\u043E\u0433\u043E, \u0449\u043E\u0431 \u043F\u043E\u0447\u0430\u043B\u0430 \u0434\u0456\u044F\u0442\u0438 \u0441\u0438\u043B\u044C\u043D\u0430 \u044F\u0434\u0435\u0440\u043D\u0430 \u0432\u0437\u0430\u0454\u043C\u043E\u0434\u0456\u044F \u0456 \u0432\u0456\u0434\u0431\u0443\u043B\u0430\u0441\u044F \u044F\u0434\u0435\u0440\u043D\u0430 \u0440\u0435\u0430\u043A\u0446\u0456\u044F, \u043F\u043E\u0442\u0440\u0456\u0431\u043D\u0430 \u0434\u0435\u044F\u043A\u0430 \u043A\u0456\u043B\u044C\u043A\u0456\u0441\u0442\u044C \u0435\u043D\u0435\u0440\u0433\u0456\u0457. \u042F\u0434\u0435\u0440\u043D\u0438\u0439 \u0441\u0438\u043D\u0442\u0435\u0437 \u0454 \u0434\u0436\u0435\u0440\u0435\u043B\u043E\u043C \u0435\u043D\u0435\u0440\u0433\u0456\u0457 \u0432 \u0437\u043E\u0440\u044F\u0445 \u0442\u0430 \u0437\u0430\u0441\u0442\u043E\u0441\u043E\u0432\u0443\u0454\u0442\u044C\u0441\u044F \u0443 \u0432\u043E\u0434\u043D\u0435\u0432\u0438\u0445 \u0431\u043E\u043C\u0431\u0430\u0445."@uk ,
"Fusio nuklearra prozesu atomiko bat da, non bi nukleo edo gehiago batzen diren beste nukleo astunago bat sortzeko. Prozesu honekin energia kopuru handia igortzen edo xurgatzen da. Fusio nuklearra modu naturalean gertatzen da izarren barnean, eta artifizialki fusioko lehergailu termonuklearretan (H lehergailuan) eta fusio erreaktore esperimentaletan. Azken aplikazio horren bidez energia iturri honi erabilera zibila eman nahi zaio, elektrizitatea sortzeko, baina oraindik fase esperimentalean dago."@eu ,
"Dalam fisika nuklir, fusi nuklir (reaksi termonuklir) adalah sebuah reaksi di mana dua inti atom bergabung membentuk satu atau lebih inti atom yang lebih besar dan partikel subatom (neutron atau proton). Perbedaan dalam massa antara reaktan dan produk dimanifestasikan sebagai pelepasan energi dalam jumlah besar. Perbedaan dalam massa ini muncul akibat perbedaan dalam energi ikatan inti atom antara sebelum dan setelah reaksi. Fusi nuklir adalah proses yang memberikan daya bagi bintang untuk bersinar."@in ,
"\u6838\u878D\u5408\u53CD\u5FDC\uFF08\u304B\u304F\u3086\u3046\u3054\u3046\u306F\u3093\u306E\u3046\u3001\uFF08\u82F1: nuclear fusion reaction\uFF09\u3068\u306F\u3001\u8EFD\u3044\u6838\u7A2E\u540C\u58EB\u304C\u878D\u5408\u3057\u3066\u3088\u308A\u91CD\u3044\u6838\u7A2E\u306B\u306A\u308B\u6838\u53CD\u5FDC\u3092\u8A00\u3046\u3002\u5358\u306B\u6838\u878D\u5408\u3068\u547C\u3070\u308C\u3001\u305D\u3046\u8A18\u8FF0\u3055\u308C\u308B\u3053\u3068\u3082\u591A\u3044\u3002\u6838\u5206\u88C2\u53CD\u5FDC\u3068\u540C\u3058\u304F\u53E4\u304F\u304B\u3089\u7814\u7A76\u3055\u308C\u3066\u3044\u308B\u3002 \u6838\u878D\u5408\u53CD\u5FDC\u3092\u9023\u7D9A\u7684\u306B\u767A\u751F\u3055\u305B\u30A8\u30CD\u30EB\u30AE\u30FC\u6E90\u3068\u3057\u3066\u5229\u7528\u3059\u308B\u6838\u878D\u5408\u7089\u3082\u53E4\u304F\u304B\u3089\u7814\u7A76\u3055\u308C\u3066\u304A\u308A\u3001\u30D5\u30A3\u30AF\u30B7\u30E7\u30F3\u4F5C\u54C1\u306B\u306F\u3088\u304F\u767B\u5834\u3059\u308B\u304C\u3001\u73FE\u5B9F\u306B\u306F\u6280\u8853\u7684\u306A\u56F0\u96E3\u3092\u4F34\u3046\u305F\u30812022\u5E74\u73FE\u5728\u5B9F\u7528\u5316\u306F\u3055\u308C\u3066\u3044\u306A\u3044 \u3002"@ja ,
"La fusi\u00F3 nuclear consisteix en una reacci\u00F3 en la qual dos nuclis at\u00F2mics (per exemple de deuteri) es converteixen en un nucli m\u00E9s pesant (en l'exemple heli), aquesta reacci\u00F3 va acompanyada de l'emissi\u00F3 de part\u00EDcules (en l'exemple del deuteri un neutr\u00F3). Aquestes reaccions poden produir una gran emissi\u00F3 d'energia, en forma de raigs gamma i d'energia cin\u00E8tica de les part\u00EDcules emeses. Aquesta emissi\u00F3 d'energia \u00E9s apreciable disminuci\u00F3 de massa per la famosa f\u00F3rmula d'Einstein E=mc\u00B2."@ca ,
"\u0422\u0435\u0440\u043C\u043E\u044F\u0301\u0434\u0435\u0440\u043D\u0430\u044F \u0440\u0435\u0430\u0301\u043A\u0446\u0438\u044F \u2014 \u0440\u0430\u0437\u043D\u043E\u0432\u0438\u0434\u043D\u043E\u0441\u0442\u044C \u044F\u0434\u0435\u0440\u043D\u043E\u0439 \u0440\u0435\u0430\u043A\u0446\u0438\u0438, \u043F\u0440\u0438 \u043A\u043E\u0442\u043E\u0440\u043E\u0439 \u043B\u0451\u0433\u043A\u0438\u0435 \u0430\u0442\u043E\u043C\u043D\u044B\u0435 \u044F\u0434\u0440\u0430 \u043E\u0431\u044A\u0435\u0434\u0438\u043D\u044F\u044E\u0442\u0441\u044F \u0432 \u0431\u043E\u043B\u0435\u0435 \u0442\u044F\u0436\u0451\u043B\u044B\u0435 \u0437\u0430 \u0441\u0447\u0451\u0442 \u043A\u0438\u043D\u0435\u0442\u0438\u0447\u0435\u0441\u043A\u043E\u0439 \u044D\u043D\u0435\u0440\u0433\u0438\u0438 \u0438\u0445 \u0442\u0435\u043F\u043B\u043E\u0432\u043E\u0433\u043E \u0434\u0432\u0438\u0436\u0435\u043D\u0438\u044F."@ru ,
"Nuclear fusion is a reaction in which two or more atomic nuclei are combined to form one or more different atomic nuclei and subatomic particles (neutrons or protons). The difference in mass between the reactants and products is manifested as either the release or absorption of energy. This difference in mass arises due to the difference in nuclear binding energy between the atomic nuclei before and after the reaction. Nuclear fusion is the process that powers active or main sequence stars and other high-magnitude stars, where large amounts of energy are released."@en ,
"Jadern\u00E1 \u010Di nukle\u00E1rn\u00ED f\u00FAze je typ jadern\u00E9 reakce, p\u0159i kter\u00E9 doch\u00E1z\u00ED ke slu\u010Dov\u00E1n\u00ED atomov\u00FDch jader leh\u010D\u00EDch prvk\u016F v j\u00E1dra t\u011B\u017E\u0161\u00EDch prvk\u016F a z\u00E1rove\u0148 k uvoln\u011Bn\u00ED energie. Termojadern\u00E1 f\u00FAze prob\u00EDhaj\u00EDc\u00ED za vysok\u00FDch teplot je zdrojem energie v\u011Bt\u0161iny hv\u011Bzd v\u010Detn\u011B Slunce. Jadern\u00E1 f\u00FAze je v principu opakem \u0161t\u011Bpen\u00ED jader t\u011B\u017Ek\u00FDch prvk\u016F."@cs ,
"Als Kernfusion werden Kernreaktionen bezeichnet, bei denen je zwei Atomkerne zu einem neuen Kern verschmelzen. Kernfusionsreaktionen sind die Ursache daf\u00FCr, dass die Sonne und alle leuchtenden Sterne Energie abstrahlen. Die oben abgebildete Fusionsreaktion als thermonuklearer Vorgang soll in Zukunft der Stromerzeugung in Kernfusionsreaktoren dienen: Kerne von Deuterium (2H) und Tritium (3H) verschmelzen zu einem Heliumkern (4He) unter Freisetzung eines Neutrons (n) sowie von Energie (3,5 MeV + 14,1 MeV)."@de ,
"Nuair a nascann dh\u00E1 n\u00FAicl\u00E9as bheaga le ch\u00E9ile chun n\u00FAicl\u00E9as n\u00EDos m\u00F3 a dh\u00E9anamh,sin comhle\u00E1 n\u00FAicl\u00E9ach. Scaoiltear fuinneamh n\u00FAicl\u00E9ach amach as n\u00FAicl\u00E9as nuair a chomhle\u00E1itear dh\u00E1 n\u00FAicl\u00E9\u00F3n n\u00F3 dh\u00E1 n\u00FAicl\u00E9as bheaga (mar shampla n\u00FAicl\u00E9as de dheoit\u00E9iriaim is n\u00FAicl\u00E9as de thritiam, dh\u00E1 iseat\u00F3p hidrigine) le ch\u00E9ile chun n\u00FAicl\u00E9as n\u00EDos m\u00F3 a chruth\u00FA. Athr\u00FA maise chuig fuinneamh is bun leis an gcruth\u00FA fuinnimh seo. I dt\u00EDortha ar fud an domhain, t\u00E1thar ag iarraidh an t-imoibri\u00FA seo a chur ar si\u00FAl ar bhonn lean\u00FAnach sti\u00FArtha chun an fuinneamh a fh\u00E1il uaidh agus cumhacht leictreach a ghini\u00FAint uaidh sin."@ga ,
"\u6838\u805A\u53D8\uFF08\u53F0\u6E7E\u7A31\u70BA\u6838\u878D\u5408\uFF09\uFF0C\uFF08\u82F1\u8A9E\uFF1ANuclear fusion\u3001 \u5FB7\u8A9E\uFF1AKernfusion\uFF09\u53C8\u7A31\u878D\u5408\u53CD\u61C9\uFF0C\u662F\u6307\u5C06\u4E24\u4E2A\u8F83\u8F7B\u7684\u6838\u7ED3\u5408\u800C\u5F62\u6210\u4E00\u4E2A\u8F83\u91CD\u7684\u6838\u548C\u4E00\u4E2A\u6975\u8F7B\u7684\u6838\uFF08\u6216\u7C92\u5B50\uFF09\u7684\u4E00\u79CD\u6838\u53CD\u5E94\u5F62\u5F0F\u3002\u5728\u6B64\u8FC7\u7A0B\u4E2D\uFF0C\u7269\u8D28\u4E26\u6CA1\u6709\u5B88\u6052\uFF0C\u56E0\u4E3A\u6709\u4E00\u90E8\u5206\u6B63\u5728\u805A\u53D8\u7684\u539F\u5B50\u6838\u7684\u7269\u8D28\u88AB\u8F6C\u5316\u4E3A\u5149\u5B50\uFF08\u80FD\u91CF\uFF09\u3002\u6838\u805A\u53D8\u662F\u7ED9\u6D3B\u8DC3\u7684\u6216\u201C\u4E3B\u5E8F\u7684\u201D\u6046\u661F\u63D0\u4F9B\u80FD\u91CF\u7684\u8FC7\u7A0B\u3002 \u4E24\u4E2A\u8F83\u8F7B\u7684\u6838\u5728\u878D\u5408\u8FC7\u7A0B\u4E2D\u4EA7\u751F\u8D28\u91CF\u8017\u640D\u800C\u91CA\u653E\u51FA\u5DE8\u5927\u7684\u80FD\u91CF\uFF0C\u4E24\u4E2A\u8F7B\u6838\u5728\u53D1\u751F\u805A\u53D8\u65F6\u867D\u7136\u56E0\u5B83\u4EEC\u90FD\u5E26\u6B63\u7535\u8377\u800C\u5F7C\u6B64\u6392\u65A5\uFF0C\u7136\u800C\u4E24\u4E2A\u80FD\u91CF\u8DB3\u591F\u9AD8\u7684\u6838\u8FCE\u9762\u76F8\u9047\uFF0C\u5B83\u4EEC\u5C31\u80FD\u76F8\u5F53\u7D27\u5BC6\u5730\u805A\u96C6\u5728\u4E00\u8D77\uFF0C\u4EE5\u81F4\u6838\u529B\u80FD\u591F\u514B\u670D\u5E93\u4ED1\u65A5\u529B\u800C\u53D1\u751F\u6838\u53CD\u5E94\uFF0C\u8FD9\u4E2A\u53CD\u5E94\u53EB\u505A\u6838\u805A\u53D8\u3002 \u8209\u4F8B\uFF1A\u4E24\u4E2A\u8CEA\u91CF\u5C0F\u7684\u539F\u5B50\uFF0C\u6BD4\u65B9\u8AAA\u5169\u500B\u6C18\u539F\u5B50\uFF0C\u5728\u4E00\u5B9A\u6761\u4EF6\u4E0B\uFF08\u5982\u8D85\u9AD8\u6E29\u548C\u9AD8\u538B\uFF09\uFF0C\u6703\u53D1\u751F\u539F\u5B50\u6838\u4E92\u76F8\u805A\u5408\u4F5C\u7528\uFF0C\u751F\u6210\u4E2D\u5B50\u548C\u6C26-3\uFF0C\u5E76\u4F34\u968F\u7740\u5DE8\u5927\u7684\u80FD\u91CF\u91CA\u653E\u3002 \u539F\u5B50\u6838\u4E2D\u8574\u85CF\u5DE8\u5927\u7684\u80FD\u91CF\u3002\u6839\u636E\u8D28\u80FD\u65B9\u7A0BE=mc2\uFF0C\u539F\u5B50\u6838\u4E4B\u6DE8\u8D28\u91CF\u53D8\u5316\uFF08\u53CD\u61C9\u7269\u8207\u751F\u6210\u7269\u4E4B\u8CEA\u91CF\u5DEE\uFF09\u9020\u6210\u80FD\u91CF\u7684\u91CA\u653E\u3002\u5982\u679C\u662F\u7531\u91CD\u7684\u539F\u5B50\u6838\u53D8\u5316\u4E3A\u8F7B\u7684\u539F\u5B50\u6838\uFF0C\u7A31\u70BA\u6838\u88C2\u53D8\uFF0C\u5982\u539F\u5B50\u5F39\u7206\u70B8\uFF1B\u5982\u679C\u662F\u7531\u8F03\u8F7B\u7684\u539F\u5B50\u6838\u53D8\u5316\u4E3A\u8F03\u91CD\u7684\u539F\u5B50\u6838\uFF0C\u7A31\u70BA\u6838\u805A\u53D8\u3002\u4E00\u822C\u4F86\u8AAA\uFF0C\u9019\u7A2E\u6838\u53CD\u5E94\u6703\u7D42\u6B62\u65BC\u9435\uFF0C\u56E0\u70BA\u5176\u539F\u5B50\u6838\u6700\u70BA\u7A69\u5B9A\u3002 \u6700\u65E9\u7684\u4EBA\u5DE5\u6838\u878D\u5408\u6280\u8853\u5728\u6C2B\u5F48\u4E0A\u5F97\u5230\u4F53\u73B0\u30021950\u5E74\u4EE3\uFF0C\u4EBA\u7C7B\u5F00\u59CB\u7814\u7A76\u7528\u4E8E\u6C11\u7528\u76EE\u7684\u7684\u53D7\u63A7\u70ED\u6838\u805A\u53D8\u3002"@zh ,
"En f\u00EDsica nuclear, la fusi\u00F3n nuclear es una reacci\u00F3n nuclear en la que varios n\u00FAcleos at\u00F3micos se unen y forman un n\u00FAcleo m\u00E1s pesado.\u200BEstas reacciones son, en general, exot\u00E9rmicas cuando ocurre entre \u00E1tomos m\u00E1s ligeros que el hierro y endot\u00E9rmicas si son m\u00E1s pesados.Esta energ\u00EDa absorbida o cedida durante la reacci\u00F3n se debe al efecto conocido como defecto de masa.Las reacciones de fusi\u00F3n, mediadas por la interacci\u00F3n nuclear fuerte, ocurren cuando los \u00E1tomos ligeros que van a fusionarse disponen de la suficiente energ\u00EDa como para vencer a las fuerzas electromagn\u00E9ticas que los repelen.Estas condiciones solo se dan a gran temperatura, cuando la materia que forman estos \u00E1tomos est\u00E1 en estado de plasma.La fusi\u00F3n nuclear es, por tanto, el proceso inverso de la fisi\u00F3n nuclear, reacci\u00F3n nuclear e"@es ,
"Reakcja termoj\u0105drowa, synteza j\u0105drowa lub fuzja j\u0105drowa \u2013 zjawisko polegaj\u0105ce na z\u0142\u0105czeniu si\u0119 dw\u00F3ch l\u017Cejszych j\u0105der w jedno ci\u0119\u017Csze. R\u00F3\u017Cne j\u0105dra atomowe maj\u0105 r\u00F3\u017Cn\u0105 energi\u0119 wi\u0105zania przypadaj\u0105c\u0105 na nukleon. Najwi\u0119ksz\u0105 energi\u0119 wi\u0105zania przypadaj\u0105c\u0105 na jeden nukleon ma izotop nikiel-62 (8,7945 MeV), w wielu publikacjach podawane jest, \u017Ce jest to izotop \u017Celaza-56. Izotop 56Fe ma najmniejsz\u0105 mas\u0119 na nukleon, gdy\u017C ma on wi\u0119kszy udzia\u0142 proton\u00F3w 26/56 = 46,43%, a w Ni 28/62 = 45,16%. Reakcja termoj\u0105drowa jest g\u0142\u00F3wnym, poza energi\u0105 grawitacyjn\u0105, \u017Ar\u00F3d\u0142em energii gwiazd."@pl ,
"Fuzio a\u016D nuklea kunfandi\u011Do (angle nuclear fusion), estas kuni\u011Do de subatomaj partikloj a\u016D nukleoj (atomkernoj) por formi pli grandajn nukleojn. Kiam fuzio okazas al nukleoj pli malgrandaj ol nukleo de fero, la maso iomete malpligrandi\u011Das dum la reakcio, kaj konverti\u011Das al elradianta energio."@eo ,
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"La fusion nucl\u00E9aire (ou thermonucl\u00E9aire) est une r\u00E9action nucl\u00E9aire dans laquelle deux noyaux atomiques s\u2019assemblent pour former un noyau plus lourd. Cette r\u00E9action est \u00E0 l\u2019\u0153uvre de mani\u00E8re naturelle dans le Soleil et la plupart des \u00E9toiles de l'Univers, dans lesquelles sont cr\u00E9\u00E9s tous les \u00E9l\u00E9ments chimiques autres que l'hydrog\u00E8ne et la majeure partie de l'h\u00E9lium. Elle est, avec la fission nucl\u00E9aire, l\u2019un des deux principaux types de r\u00E9actions nucl\u00E9aires appliqu\u00E9es."@fr ,
"( \uB2E4\uB978 \uB73B\uC5D0 \uB300\uD574\uC11C\uB294 \uD575\uC735\uD569 (\uB3D9\uC74C\uC774\uC758) \uBB38\uC11C\uB97C \uCC38\uACE0\uD558\uC2ED\uC2DC\uC624.)( \uC774 \uBB38\uC11C\uB294 \uD575\uC735\uD569\uC5D0 \uAD00\uD55C \uAC83\uC785\uB2C8\uB2E4. \uC804\uB825 \uC0DD\uC0B0\uC744 \uC704\uD55C \uD575\uC735\uD569 \uBC0F \uC81C\uC5B4 \uBC29\uC2DD\uC5D0 \uB300\uD574\uC11C\uB294 \uD575\uC735\uD569 \uBC1C\uC804 \uBB38\uC11C\uB97C \uCC38\uACE0\uD558\uC2ED\uC2DC\uC624.)\n\uD575\uC735\uD569(\u6838\u878D\u5408, \uC601\uC5B4: nuclear fusion)\uC740 \uBB3C\uB9AC\uD559\uC5D0\uC11C \uD575\uBD84\uC5F4\uACFC \uC0C1\uBC18\uB418\uB294 \uD604\uC0C1\uC73C\uB85C, \uB450 \uAC1C\uC758 \uC6D0\uC790\uD575\uC774 \uBD80\uB52A\uD600 \uC0C8\uB85C\uC6B4 \uD558\uB098\uC758 \uBB34\uAC70\uC6B4 \uC6D0\uC790\uD575\uC73C\uB85C \uBCC0\uD658\uB418\uB294 \uBC18\uC751\uC774\uB2E4. \uAE30\uBCF8\uC801\uC73C\uB85C \uC6D0\uC790\uD575\uC740 \uB0B4\uBD80\uC758 \uC591\uC131\uC790\uB85C \uC778\uD574 \uC591\uC804\uD558\uB97C \uB760\uBBC0\uB85C \uB450 \uAC1C\uC758 \uC6D0\uC790\uD575\uC774 \uC11C\uB85C \uC811\uADFC\uD558\uAC8C \uB418\uBA74 \uC804\uAE30\uC801\uC778 \uCC99\uB825\uC5D0 \uC758\uD574 \uC11C\uB85C \uBC00\uC5B4\uB0B4\uAC8C \uB41C\uB2E4. \uD558\uC9C0\uB9CC \uC6D0\uC790\uD575\uC744 \uCD08\uACE0\uC628\uC73C\uB85C \uAC00\uC5F4\uD558\uBA74 \uC6D0\uC790\uD575\uC758 \uC6B4\uB3D9\uC5D0\uB108\uC9C0\uAC00 \uC804\uAE30\uC801 \uCC99\uB825\uC744 \uC774\uACA8\uB0B4\uC5B4 \uB450 \uC6D0\uC790\uD575\uC774 \uC11C\uB85C \uCDA9\uB3CC\uD558\uAC8C \uB41C\uB2E4. \uADF8\uB9AC\uACE0 \uC774\uD6C4\uC5D0\uB294 \uB450 \uC6D0\uC790\uD575 \uC0AC\uC774\uC5D0 \uAC15\uB825\uD55C \uC778\uB825\uC774 \uC791\uC6A9\uD574 \uD558\uB098\uC758 \uC6D0\uC790\uD575\uC73C\uB85C \uACB0\uD569\uB420 \uC218 \uC788\uB2E4. \uAC00\uC7A5 \uAC00\uBCBC\uC6B4 \uC6D0\uC18C\uC778 \uC218\uC18C\uC758 \uC6D0\uC790\uD575\uB07C\uB9AC \uD575\uC735\uD569\uC744 \uC704\uD574 \uD544\uC694\uD55C \uC628\uB3C4\uB294 \uB300\uB7B5 1\uC5B5\u2103(\u2103) \uC774\uC0C1\uC774\uBA70, \uB354 \uBB34\uAC70\uC6B4 \uC6D0\uC790\uD575\uB4E4 \uAC04\uC758 \uD575\uC735\uD569\uC5D0\uB294 \uB354 \uACE0\uC628\uC758 \uD658\uACBD\uC774 \uD544\uC694\uD558\uB2E4. \uB2E4\uC74C\uC740 \uAC00\uC7A5 \uAC00\uBCBC\uC6B4 \uC6D0\uC18C\uC778 \uC218\uC18C\uB97C \uD65C\uC6A9\uD55C \uD575\uC735\uD569\uBC18\uC751\uC758 \uB300\uD45C\uC801\uC778 \uC138 \uAC00\uC9C0 \uC720\uD615\uC774\uB2E4 1. 2. 3. *D\uB294 \uC911\uC218\uC18C, T\uB294 \uC0BC\uC911\uC218\uC18C, 2\uC640 3\uC758 \uBC18\uC751\uC740 \uAC01\uAC01 50%\uC758 \uD655\uB960\uB85C \uC77C\uC5B4\uB09C\uB2E4."@ko ,
"Kernfusie is in de natuurkunde het samensmelten van atoomkernen, waarbij een zwaardere atoomkern met een hoger atoomnummer (en dus een ander chemisch element) wordt gevormd. Als lichte atomen zoals deuterium, een isotoop van waterstof, samensmelten, is de natuurkundige wet van behoud van massa niet van toepassing, omdat een deel van de interne bindingsenergie vrijkomt. Deze bindingsenergie maakt een meetbaar deel uit van de massa van een atoomkern, in overeenstemming met Einsteins formule: E = mc\u00B2 (massa en energie kunnen in elkaar worden omgezet). De nieuwgevormde atoomkernen zijn hierdoor samen lichter dan de som van de massa's van de oorspronkelijke lichte kernen. Omdat de vrijgekomen energie gelijk is aan de verloren bindingsenergie, blijft bij kernfusie de wet van behoud van energie w"@nl ,
"In chimica nucleare e in fisica nucleare, la fusione nucleare \u00E8 una reazione nucleare nella quale i nuclei di due o pi\u00F9 atomi si uniscono tra loro formando il nucleo di un nuovo elemento chimico. Perch\u00E9 la fusione sia possibile i nuclei devono essere avvicinati tra loro, impiegando una grande energia per superare la repulsione elettromagnetica. La fusione degli elementi fino ai numeri atomici 26 e 28 (ferro e nichel) \u00E8 una reazione esotermica, cio\u00E8 emette energia poich\u00E9 il nucleo prodotto dalla reazione ha massa minore della somma delle masse dei nuclei reagenti. Per gli atomi con numeri atomici superiori la reazione invece \u00E8 endotermica, cio\u00E8 assorbe energia. Alcune reazioni (in primo luogo quelle con una soglia di energia pi\u00F9 bassa, come la fusione di deuterio e trizio) determinano il ri"@it ,
"Fus\u00E3o nuclear \u00E9 o processo no qual dois ou mais n\u00FAcleos at\u00F4micos se juntam e formam um outro n\u00FAcleo de maior n\u00FAmero at\u00F4mico. A fus\u00E3o nuclear requer muita energia para acontecer, e geralmente libera muito mais energia do que a que consome. Quando ocorre com elementos mais leves que o ferro e o n\u00EDquel (que possuem as maiores for\u00E7as de coes\u00E3o nuclear de todos os \u00E1tomos, sendo portanto mais est\u00E1veis) ela geralmente libera energia, e com elementos mais pesados ela consome. At\u00E9 hoje, in\u00EDcio do s\u00E9culo XXI, ainda n\u00E3o foi encontrada uma forma de controlar comercialmente a fus\u00E3o nuclear, como acontece com a fiss\u00E3o, embora existam laborat\u00F3rios de pesquisa que utilizam reatores de fus\u00E3o nuclear em pesquisas cient\u00EDficas. Um projeto que caminha para a demonstra\u00E7\u00E3o da viabilidade comercial do uso da fus\u00E3"@pt ;
owl:differentFrom dbr:Nuclear_fission ;
rdfs:seeAlso dbr:Abundance_of_the_chemical_elements ,
dbr:CNO_cycle ,
,
dbr:Aneutronic_fusion ,
,
dbr:Abundance_of_elements ;
foaf:depiction ,
,
,
,
,
,
,
.
@prefix dcterms: .
@prefix dbc: .
dbr:Nuclear_fusion dcterms:subject dbc:Nuclear_physics ,
dbc:Energy_conversion ,
dbc:Nuclear_chemistry ,
dbc:Neutron_sources ,
dbc:Physical_phenomena ,
dbc:Nuclear_fusion ;
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"En f\u00EDsica nuclear, la fusi\u00F3n nuclear es una reacci\u00F3n nuclear en la que varios n\u00FAcleos at\u00F3micos se unen y forman un n\u00FAcleo m\u00E1s pesado.\u200BEstas reacciones son, en general, exot\u00E9rmicas cuando ocurre entre \u00E1tomos m\u00E1s ligeros que el hierro y endot\u00E9rmicas si son m\u00E1s pesados.Esta energ\u00EDa absorbida o cedida durante la reacci\u00F3n se debe al efecto conocido como defecto de masa.Las reacciones de fusi\u00F3n, mediadas por la interacci\u00F3n nuclear fuerte, ocurren cuando los \u00E1tomos ligeros que van a fusionarse disponen de la suficiente energ\u00EDa como para vencer a las fuerzas electromagn\u00E9ticas que los repelen.Estas condiciones solo se dan a gran temperatura, cuando la materia que forman estos \u00E1tomos est\u00E1 en estado de plasma.La fusi\u00F3n nuclear es, por tanto, el proceso inverso de la fisi\u00F3n nuclear, reacci\u00F3n nuclear en la que un \u00E1tomo pesado da lugar a dos \u00E1tomos m\u00E1s ligeros.\u200B Dada la temperatura necesaria, en la naturaleza este tipo de reacciones solo pueden observarse en el n\u00FAcleo de las estrellas, donde las temperaturas son del orden de decenas de millones de Kelvin.La energ\u00EDa liberada en las reacciones de fusi\u00F3n que ocurren en las estrellas es, de hecho, la principal fuente de energ\u00EDa de estas.Adem\u00E1s, estas reacciones de fusi\u00F3n que ocurren en las estrellas son una de las principales fuentes de creaci\u00F3n de los elementos qu\u00EDmicos pesados existentes en la naturaleza, en un proceso conocido como nucleos\u00EDntesis estelar.\u200B Artificialmente tambi\u00E9n pueden llevarse a cabo reacciones de fusi\u00F3n, aunque debido a las condiciones de temperatura necesarias, el control de estas reacciones es un reto tecnol\u00F3gico a\u00FAn no resuelto.La primera aplicaci\u00F3n de la fusi\u00F3n nuclear llevada a la pr\u00E1ctica fue la invenci\u00F3n de la bomba de hidr\u00F3geno.En la actualidad tambi\u00E9n se investiga c\u00F3mo mantener las condiciones necesarias para que ocurran las reacciones de fusi\u00F3n nuclear de manera controlada y poder as\u00ED generar energ\u00EDa el\u00E9ctrica a partir de ella.En particular, dado que la energ\u00EDa liberada durante la reacci\u00F3n es mayor cuanto menor sea la masa de los \u00E1tomos intervinientes, suelen investigarse las reacciones de fusi\u00F3n que ocurren entre distintos is\u00F3topos del hidr\u00F3geno.Para el control de la reacci\u00F3n existen distintos conceptos en desarrollo, fundamentalmente el confinamiento inercial y el confinamiento magn\u00E9tico.Esta investigaci\u00F3n se lleva a cabo en distintos laboratorios y organizaciones del mundo, siendo la m\u00E1s destacada el proyecto ITER fruto de la colaboraci\u00F3n internacional y centrado en el confinamiento magn\u00E9tico.\u200B"@es ,
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"K\u00E4rnfusion \u00E4r den process d\u00E5 atomk\u00E4rnor sm\u00E4lter samman och bildar st\u00F6rre och tyngre k\u00E4rnor. P\u00E5 grund av de sm\u00E5 atomk\u00E4rnornas l\u00E5ga bindningsenergi per nukleon kan man \"tj\u00E4na\" (frig\u00F6ra) energi om man sl\u00E5r ihop tv\u00E5 sm\u00E5 k\u00E4rnor till en tyngre. I stj\u00E4rnor f\u00F6rekommer k\u00E4rnfusion i mitten av stj\u00E4rnan, och det \u00E4r detta som \u00E4r deras energik\u00E4lla. P\u00E5 jorden f\u00F6rekommer fusion i st\u00F6rre omfattning endast i v\u00E4tebomber, men mycket pengar och forskning har lagts ner p\u00E5 att kunna anv\u00E4nda fusion som praktisk anv\u00E4ndbar energik\u00E4lla, precis vad som har skett med fission (k\u00E4rnklyvning). F\u00F6r att fusion ska kunna ske m\u00E5ste f\u00F6rst extrema temperaturer och tryck uppn\u00E5s, vilket bland annat den planerade reaktorn ITER ska f\u00F6rs\u00F6ka \u00E5stadkomma. Att kunna genomf\u00F6ra fusion under mindre extrema f\u00F6rh\u00E5llanden och skala vore en uppt\u00E4ckt med \u00E4nnu l\u00E4ngre g\u00E5ende konsekvenser f\u00F6r v\u00E4rldens energif\u00F6rs\u00F6rjning, se vidare kall fusion. Ur fusionsprocessen kommer energi framf\u00F6rallt ut som kinetisk energi f\u00F6r k\u00E4rnor, neutroner och andra partiklar. Dessutom frig\u00F6rs en del gammastr\u00E5lning. Ordet fusion f\u00F6rekommer i svensk media sedan 1952."@sv ,
"Jadern\u00E1 \u010Di nukle\u00E1rn\u00ED f\u00FAze je typ jadern\u00E9 reakce, p\u0159i kter\u00E9 doch\u00E1z\u00ED ke slu\u010Dov\u00E1n\u00ED atomov\u00FDch jader leh\u010D\u00EDch prvk\u016F v j\u00E1dra t\u011B\u017E\u0161\u00EDch prvk\u016F a z\u00E1rove\u0148 k uvoln\u011Bn\u00ED energie. Termojadern\u00E1 f\u00FAze prob\u00EDhaj\u00EDc\u00ED za vysok\u00FDch teplot je zdrojem energie v\u011Bt\u0161iny hv\u011Bzd v\u010Detn\u011B Slunce. Jadern\u00E1 f\u00FAze je v principu opakem \u0161t\u011Bpen\u00ED jader t\u011B\u017Ek\u00FDch prvk\u016F. Proti slu\u010Dov\u00E1n\u00ED jader p\u016Fsob\u00ED odpudiv\u00E1 elektrick\u00E1 interakce (ob\u011B j\u00E1dra jsou kladn\u011B nabit\u00E1). Dostanou-li se v\u0161ak lehk\u00E1 j\u00E1dra dostate\u010Dn\u011B bl\u00EDzko k sob\u011B, aby p\u0159ekonala , p\u0159evl\u00E1dne nad elektrickou silou p\u0159ita\u017Eliv\u00E1 jadern\u00E1 s\u00EDla a ob\u011B j\u00E1dra se slou\u010D\u00ED. Rozd\u00EDl mezi klidov\u00FDmi hmotnostmi jader p\u0159ed a po slou\u010Den\u00ED se uvoln\u00ED ve form\u011B energie."@cs ,
"Reakcja termoj\u0105drowa, synteza j\u0105drowa lub fuzja j\u0105drowa \u2013 zjawisko polegaj\u0105ce na z\u0142\u0105czeniu si\u0119 dw\u00F3ch l\u017Cejszych j\u0105der w jedno ci\u0119\u017Csze. R\u00F3\u017Cne j\u0105dra atomowe maj\u0105 r\u00F3\u017Cn\u0105 energi\u0119 wi\u0105zania przypadaj\u0105c\u0105 na nukleon. Najwi\u0119ksz\u0105 energi\u0119 wi\u0105zania przypadaj\u0105c\u0105 na jeden nukleon ma izotop nikiel-62 (8,7945 MeV), w wielu publikacjach podawane jest, \u017Ce jest to izotop \u017Celaza-56. Izotop 56Fe ma najmniejsz\u0105 mas\u0119 na nukleon, gdy\u017C ma on wi\u0119kszy udzia\u0142 proton\u00F3w 26/56 = 46,43%, a w Ni 28/62 = 45,16%. W wyniku reakcji egzotermicznej wydzielona energia (w postaci energii kinetycznej produkt\u00F3w i promieniowania gamma), zostaje rozproszona na otaczaj\u0105cych atomach i przekszta\u0142ca si\u0119 na energi\u0119 ciepln\u0105. Energi\u0119 wydzielaj\u0105c\u0105 si\u0119 podczas reakcji mo\u017Cna wyznaczy\u0107 bez przeprowadzania reakcji na podstawie deficytu masy, czyli r\u00F3\u017Cnicy mas sk\u0142adnik\u00F3w i produkt\u00F3w reakcji. J\u0105dra atomowe maj\u0105 dodatni \u0142adunek elektryczny i dlatego si\u0119 odpychaj\u0105 \u2013 aby dosz\u0142o do ich po\u0142\u0105czenia, musz\u0105 zbli\u017Cy\u0107 si\u0119 na tyle, aby si\u0142y oddzia\u0142ywa\u0144 j\u0105drowych pokona\u0142y odpychanie elektrostatyczne. Niezb\u0119dnym warunkiem do tego jest pr\u0119dko\u015B\u0107 (energia kinetyczna) j\u0105der. Wysok\u0105 energi\u0119 j\u0105der uzyskuje si\u0119 w bardzo wysokich temperaturach lub rozp\u0119dzaj\u0105c j\u0105dra w akceleratorach cz\u0105stek. Przedrostek termo pochodzi od g\u0142\u00F3wnego sposobu, w jaki wywo\u0142ywana jest ta reakcja w gwiazdach i bombie wodorowej, czyli przez podniesienie temperatury do kilkunastu milion\u00F3w kelwin\u00F3w. W skali atomowej oznacza to bardzo du\u017C\u0105 energi\u0119 zderzenia cz\u0105stek. Istnieje hipoteza, \u017Ce synteza j\u0105drowa mo\u017Ce zachodzi\u0107 r\u00F3wnie\u017C w ni\u017Cszych temperaturach (zimna fuzja). Reakcja termoj\u0105drowa jest g\u0142\u00F3wnym, poza energi\u0105 grawitacyjn\u0105, \u017Ar\u00F3d\u0142em energii gwiazd."@pl ,
"Fus\u00E3o nuclear \u00E9 o processo no qual dois ou mais n\u00FAcleos at\u00F4micos se juntam e formam um outro n\u00FAcleo de maior n\u00FAmero at\u00F4mico. A fus\u00E3o nuclear requer muita energia para acontecer, e geralmente libera muito mais energia do que a que consome. Quando ocorre com elementos mais leves que o ferro e o n\u00EDquel (que possuem as maiores for\u00E7as de coes\u00E3o nuclear de todos os \u00E1tomos, sendo portanto mais est\u00E1veis) ela geralmente libera energia, e com elementos mais pesados ela consome. At\u00E9 hoje, in\u00EDcio do s\u00E9culo XXI, ainda n\u00E3o foi encontrada uma forma de controlar comercialmente a fus\u00E3o nuclear, como acontece com a fiss\u00E3o, embora existam laborat\u00F3rios de pesquisa que utilizam reatores de fus\u00E3o nuclear em pesquisas cient\u00EDficas. Um projeto que caminha para a demonstra\u00E7\u00E3o da viabilidade comercial do uso da fus\u00E3o nuclear controlada \u00E9 o ITER. O principal tipo de fus\u00E3o que ocorre no interior das estrelas \u00E9 o de hidrog\u00EAnio em h\u00E9lio, onde quatro pr\u00F3tons se fundem em uma part\u00EDcula alfa (um n\u00FAcleo de h\u00E9lio), liberando dois p\u00F3sitrons, dois neutrinos e energia. Mas, dentro desse processo, ocorrem v\u00E1rias rea\u00E7\u00F5es individuais, que variam de acordo com a massa da estrela. Para estrelas do tamanho do Sol ou menores, a cadeia pr\u00F3ton-pr\u00F3ton \u00E9 a rea\u00E7\u00E3o dominante. Em estrelas de massa elevada predomina o ciclo CNO. A fus\u00E3o de deut\u00E9rio e tr\u00EDtio (is\u00F3topos do hidrog\u00EAnio) pode gerar n\u00EAutrons, o que \u00E9 perigoso e torna o processo menos eficaz. A fus\u00E3o aneutr\u00F4nica (sem gera\u00E7\u00E3o de n\u00EAutrons) \u00E9 poss\u00EDvel com o uso de elementos como o h\u00E9lio-3 (raro na Terra), l\u00EDtio e boro (abundantes na superf\u00EDcie terrestre), entre outros. Vale ressaltar que h\u00E1 conserva\u00E7\u00E3o da energia, e, portanto, pode-se calcular a massa dos quatro pr\u00F3tons e do n\u00FAcleo de h\u00E9lio, e subtrair a soma das massas das part\u00EDculas iniciais daquela do produto desta rea\u00E7\u00E3o nuclear para calcular a energia produzida. Utilizando a equa\u00E7\u00E3o E=mc\u00B2, pode-se calcular a energia liberada, oriunda da diferen\u00E7a de massas. Uma vez que o valor de c \u00E9 muito grande (cerca de 3\u00D7108 m/s), mesmo uma massa muito pequena corresponde a uma enorme quantidade de energia. Este fato levou muitos engenheiros e cientistas a iniciar projetos para o desenvolvimento de reatores de fus\u00E3o (Tokamaks) de modo a gerar eletricidade (por exemplo, a fus\u00E3o de poucos cm\u00B3 de deut\u00E9rio, um is\u00F3topo de hidrog\u00EAnio, produziria uma energia equivalente \u00E0quela produzida pela queima de 20 toneladas de carv\u00E3o)."@pt ,
"Kernfusie is in de natuurkunde het samensmelten van atoomkernen, waarbij een zwaardere atoomkern met een hoger atoomnummer (en dus een ander chemisch element) wordt gevormd. Als lichte atomen zoals deuterium, een isotoop van waterstof, samensmelten, is de natuurkundige wet van behoud van massa niet van toepassing, omdat een deel van de interne bindingsenergie vrijkomt. Deze bindingsenergie maakt een meetbaar deel uit van de massa van een atoomkern, in overeenstemming met Einsteins formule: E = mc\u00B2 (massa en energie kunnen in elkaar worden omgezet). De nieuwgevormde atoomkernen zijn hierdoor samen lichter dan de som van de massa's van de oorspronkelijke lichte kernen. Omdat de vrijgekomen energie gelijk is aan de verloren bindingsenergie, blijft bij kernfusie de wet van behoud van energie wel gelden. Het fuseren van zwaardere atomen kost energie. De overgang tussen 'licht' en 'zwaar' ligt in dit verband bij het element ijzer. Voordat in 1938 de Duitse fysicus Hans Bethe het idee opperde dat de zon en de sterren hun energie opwekken door kernfusie, was het een raadsel waar al die energie vandaan kwam. Alle in die tijd bekende chemische reacties leverden daarvoor veel te weinig energie op. De zon zet per seconde ongeveer 700 miljoen ton waterstof via kernfusie om in circa 695 miljoen ton helium. Het massaverlies, rond de 4,4 miljoen ton, komt overeen met de vrijgekomen bindingsenergie. In lichte sterren (zoals de zon) verloopt de kernfusie van waterstofatomen volgens de proton-protoncyclus, in zwaardere volgens de koolstof-stikstofcyclus. In oudere sterren volgt na het opbranden van de beschikbare waterstof vaak het triple-alfaproces, waarbij uiteindelijk koolstof wordt gevormd. Omdat atoomkernen positief geladen zijn, stoten ze elkaar elektrostatisch af - pas als de kernen elkaar heel dicht naderen wordt de (aantrekkende) sterke kernkracht belangrijk genoeg om tot kernfusie te leiden. Alleen bij extreem hoge temperatuur en druk, zoals die heersen in het middelpunt van sterren, hebben de deeltjes voldoende energie om de afstotende elektrostatische kracht te overwinnen. Op aarde zijn zulke omstandigheden niet eenvoudig na te bootsen, en technologische toepassing van het kernfusieprincipe is dan ook niet wijdverbreid. Kernfusie heeft echter wel een enorm potentieel als energiebron, omdat er grote hoeveelheden lichte kernen op aarde aanwezig zijn (met name waterstof en isotopen daarvan), waardoor de brandstof vrijwel eindeloos voorradig is. Daarnaast komen er geen broeikasgassen vrij en minder radioactief afval dan bij kernsplijting. Daarom proberen wetenschappers kernfusie op aarde te ontwikkelen als schone en veilige energiebron. Hoewel hiermee grote vorderingen gemaakt zijn en de omstandigheden voor kernfusie inmiddels routinematig kunnen worden gecre\u00EBerd in gespecialiseerde laboratoria, is er anno 2020 nog geen prototype dat daadwerkelijk energie produceert. Zie fusie-energie voor meer informatie over dit onderwerp. Daarnaast levert bij vrijwel alle huidige kernwapens kernfusie de meeste energie, behalve eventueel bij een splijting-fusie-splijting ontwerp (zie: waterstofbom). Hierbij cre\u00EBert een bom gebaseerd op kernsplijting de extreme omstandigheden die nodig zijn om de fusie-reactie in gang te zetten en fungeert dus in feite als de ontsteker. Dit proces is echter niet eenvoudig in te zetten voor vreedzame toepassingen of energieopwekking."@nl ,
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\uC774\uC0C1\uC774\uBA70, \uB354 \uBB34\uAC70\uC6B4 \uC6D0\uC790\uD575\uB4E4 \uAC04\uC758 \uD575\uC735\uD569\uC5D0\uB294 \uB354 \uACE0\uC628\uC758 \uD658\uACBD\uC774 \uD544\uC694\uD558\uB2E4. \uC9C0\uAD6C\uC758 \uC6D0\uC18C\uB4E4 \uC911, \uCCA0\uC758 \uC6D0\uC790\uD575\uC740 \uBAA8\uB4E0 \uC6D0\uC790\uD575 \uAC00\uC6B4\uB370 \uAC00\uC7A5 \uAC15\uD55C \uACB0\uD569 \uC5D0\uB108\uC9C0\uB97C \uAC00\uC9C0\uACE0 \uC788\uC73C\uBA70, \uAC00\uC7A5 \uC548\uC815\uB418\uC5B4 \uC788\uB2E4. \uADF8\uB7EC\uBBC0\uB85C, \uCCA0\uBCF4\uB2E4 \uAC00\uBCBC\uC6B4 \uC6D0\uC790\uD575\uB4E4 \uC0AC\uC774\uC758 \uD575\uC735\uD569 \uBC18\uC751\uC5D0\uC11C\uB294 \uC77C\uBC18\uC801\uC73C\uB85C \uC8FC\uBCC0\uC73C\uB85C \uC5D0\uB108\uC9C0\uB97C \uBC29\uCD9C\uD558\uBA70, \uCCA0\uBCF4\uB2E4 \uBB34\uAC70\uC6B4 \uC6D0\uC790\uD575\uB4E4 \uC0AC\uC774\uC758 \uD575\uC735\uD569 \uBC18\uC751\uC5D0\uC11C\uB294 \uC8FC\uBCC0\uC73C\uB85C\uBD80\uD130 \uC5D0\uB108\uC9C0\uB97C \uD761\uC218\uD55C\uB2E4. \uB2E4\uC74C\uC740 \uAC00\uC7A5 \uAC00\uBCBC\uC6B4 \uC6D0\uC18C\uC778 \uC218\uC18C\uB97C \uD65C\uC6A9\uD55C \uD575\uC735\uD569\uBC18\uC751\uC758 \uB300\uD45C\uC801\uC778 \uC138 \uAC00\uC9C0 \uC720\uD615\uC774\uB2E4 1. 2. 3. *D\uB294 \uC911\uC218\uC18C, T\uB294 \uC0BC\uC911\uC218\uC18C, 2\uC640 3\uC758 \uBC18\uC751\uC740 \uAC01\uAC01 50%\uC758 \uD655\uB960\uB85C \uC77C\uC5B4\uB09C\uB2E4. \uD575\uC735\uD569 \uBC1C\uC804\uC740 \uC704\uC640 \uAC19\uC740 \uC218\uC18C\uC758 \uD575\uC735\uD569\uBC18\uC751 \uC2DC \uBC1C\uC0DD\uB418\uB294 \uC5D0\uB108\uC9C0\uB97C \uD65C\uC6A9\uD574 \uC804\uAE30\uB97C \uC0DD\uC0B0\uD558\uB294 \uBC1C\uC804\uBC29\uC2DD\uC774\uB2E4. \uD654\uB825\uBC1C\uC804\uC774\uB098 \uC6D0\uC790\uB825\uBC1C\uC804\uC5D0 \uBE44\uD574 \uC5D0\uB108\uC9C0 \uC0DD\uC0B0\uB7C9\uC774 \uD6E8\uC52C \uB9CE\uACE0 \uD658\uACBD\uC624\uC5FC \uBB3C\uC9C8\uC744 \uBC1C\uC0DD\uC2DC\uD0A4\uC9C0 \uC54A\uB294 \uC7A5\uC810 \uB54C\uBB38\uC5D0 \uD604\uC7AC \uB9CE\uC740 \uB098\uB77C\uC758 \uC5F0\uAD6C\uAE30\uAD00\uB4E4\uC774 \uAD6D\uAC00\uC801 \uB610\uB294 \uAD6D\uC81C\uC801 \uCC28\uC6D0\uC5D0\uC11C \uD65C\uBC1C\uD788 \uC5F0\uAD6C\uB97C \uC218\uD589\uD558\uACE0 \uC788\uB2E4. \uAD6D\uC81C\uC5F4\uD575\uC735\uD569\uC2E4\uD5D8\uB85C(ITER) \uD504\uB85C\uC81D\uD2B8\uAC00 \uB300\uD45C\uC801\uC73C\uB85C, \uB300\uD55C\uBBFC\uAD6D\uC744 \uD3EC\uD568\uD55C 7\uAC1C\uAD6D\uC774 \uCC38\uC5EC\uD558\uACE0 \uC788\uB2E4. \uD575\uC735\uD569\uC740 \uD0DC\uC591\uC758 \uC5D0\uB108\uC9C0\uC6D0\uC73C\uB85C\uB3C4 \uC798 \uC54C\uB824\uC838 \uC788\uB294\uB370, \uD0DC\uC591\uC744 \uD3EC\uD568\uD558\uC5EC \uB300\uBD80\uBD84\uC758 \uD56D\uC131\uC5D0\uC11C \uC77C\uC5B4\uB098\uB294 \uD575\uC735\uD569\uBC18\uC751\uC740 \uC218\uC18C\uC6D0\uC790\uB97C \uC911\uC218\uC18C(Deuterium) \uB610\uB294 \uC0BC\uC911\uC218\uC18C(Tritium)\uB85C \uC735\uD569\uD558\uACE0, \uC774\uB4E4\uC744 \uD5EC\uB968 \uC6D0\uC790\uB85C \uC735\uD569\uC2DC\uD0A4\uB294 \uC5F0\uC18D\uC801\uC778 \uD575\uC735\uD569\uBC18\uC751\uC774\uB2E4. \uBB34\uAC70\uC6B4 \uC6D0\uC18C\uC758 \uD575\uC735\uD569\uC740 \uCD08\uC2E0\uC131 \uD3ED\uBC1C\uACFC \uAC19\uC740 \uADF9\uB2E8\uC801\uC778 \uACBD\uC6B0\uC5D0 \uBC1C\uC0DD\uD55C\uB2E4. \uD56D\uC131 \uBC0F \uCD08\uC2E0\uC131\uC5D0\uC11C\uC758 \uD575\uC735\uD569\uC740 \uC790\uC5F0\uC801\uC73C\uB85C \uC874\uC7AC\uD558\uB294 \uC6D0\uC18C\uAC00 \uB9CC\uB4E4\uC5B4\uC9C4 \uAC00\uC7A5 \uC8FC\uC694\uD55C \uC6D0\uC778\uC774\uB2E4. \uC6D0\uC790\uD575\uC744 \uC11C\uB85C \uC735\uD569\uD558\uAC8C \uD558\uB294 \uAC83\uC740 \uC544\uC8FC \uB9CE\uC740 \uC5D0\uB108\uC9C0\uB97C \uD544\uC694\uB85C \uD55C\uB2E4. \uC774\uB294 \uAC00\uC7A5 \uAC00\uBCBC\uC6B4 \uC6D0\uC18C\uC778 \uC218\uC18C\uC5D0 \uB300\uD574\uC11C\uB3C4 \uC0AC\uC2E4\uC0C1 \uB9C8\uCC2C\uAC00\uC9C0\uC774\uB2E4. \uD558\uC9C0\uB9CC \uAC00\uBCBC\uC6B4 \uC6D0\uC18C\uAC00 \uC735\uD569\uD574\uC11C \uBB34\uAC70\uC6B4 \uC6D0\uC18C \uBC0F \uC790\uC720 \uC911\uC131\uC790\uB97C \uB9CC\uB4E4 \uB54C, \uC774 \uACFC\uC815\uC5D0\uC11C \uBC1C\uC0DD\uD558\uB294 \uC5D0\uB108\uC9C0\uB294 \uC735\uD569\uD558\uB294 \uB370 \uD544\uC694\uB85C \uD588\uB358 \uC5D0\uB108\uC9C0 \uC774\uC0C1\uC774\uB2E4. \uC774\uB7EC\uD55C \uC5D0\uB108\uC9C0 \uC0DD\uC131 \uACFC\uC815, \uC989 \uBC1C\uC5F4\uBC18\uC751\uC740 \uD575\uC735\uD569 \uBC18\uC751\uC774 \uC2A4\uC2A4\uB85C \uC9C0\uC18D\uB420 \uC218 \uC788\uB3C4\uB85D \uD55C\uB2E4. \uB300\uBD80\uBD84\uC758 \uD575\uBC18\uC751\uC5D0\uC11C \uBC1C\uC0DD\uD558\uB294 \uC5D0\uB108\uC9C0\uB294 \uD654\uD559 \uBC18\uC751\uC5D0 \uC758\uD574 \uBC1C\uC0DD\uD558\uB294 \uC5D0\uB108\uC9C0\uC5D0 \uBE44\uD574 \uB9E4\uC6B0 \uD06C\uB2E4. \uC774\uB294 \uC6D0\uC790\uD575\uC744 \uD568\uAED8 \uBAA8\uC544\uC8FC\uB294 \uACB0\uD569 \uC5D0\uB108\uC9C0\uAC00 \uC804\uC790\uC640 \uC6D0\uC790\uD575\uC744 \uBAA8\uC544\uC8FC\uB294 \uC5D0\uB108\uC9C0\uBCF4\uB2E4 \uD6E8\uC52C \uD06C\uAE30 \uB54C\uBB38\uC774\uB2E4. \uC608\uB97C \uB4E4\uC5B4, \uC804\uC790\uB97C \uC218\uC18C\uC5D0 \uBD99\uC5EC\uC11C \uC5BB\uB294 \uC774\uC628\uD654 \uC5D0\uB108\uC9C0\uB294 13.6eV\uC774\uBA70, \uC774\uB294 \uC911\uC218\uC18C-\uC0BC\uC911\uC218\uC18C(D-T) \uBC18\uC751\uC5D0\uC11C \uBC1C\uC0DD\uD558\uB294 17MeV\uC758 \uBC31\uB9CC\uBD84\uC758 \uC77C\uC870\uCC28\uB3C4 \uB418\uC9C0 \uC54A\uB294\uB2E4."@ko ,
"\u6838\u878D\u5408\u53CD\u5FDC\uFF08\u304B\u304F\u3086\u3046\u3054\u3046\u306F\u3093\u306E\u3046\u3001\uFF08\u82F1: nuclear fusion reaction\uFF09\u3068\u306F\u3001\u8EFD\u3044\u6838\u7A2E\u540C\u58EB\u304C\u878D\u5408\u3057\u3066\u3088\u308A\u91CD\u3044\u6838\u7A2E\u306B\u306A\u308B\u6838\u53CD\u5FDC\u3092\u8A00\u3046\u3002\u5358\u306B\u6838\u878D\u5408\u3068\u547C\u3070\u308C\u3001\u305D\u3046\u8A18\u8FF0\u3055\u308C\u308B\u3053\u3068\u3082\u591A\u3044\u3002\u6838\u5206\u88C2\u53CD\u5FDC\u3068\u540C\u3058\u304F\u53E4\u304F\u304B\u3089\u7814\u7A76\u3055\u308C\u3066\u3044\u308B\u3002 \u6838\u878D\u5408\u53CD\u5FDC\u3092\u9023\u7D9A\u7684\u306B\u767A\u751F\u3055\u305B\u30A8\u30CD\u30EB\u30AE\u30FC\u6E90\u3068\u3057\u3066\u5229\u7528\u3059\u308B\u6838\u878D\u5408\u7089\u3082\u53E4\u304F\u304B\u3089\u7814\u7A76\u3055\u308C\u3066\u304A\u308A\u3001\u30D5\u30A3\u30AF\u30B7\u30E7\u30F3\u4F5C\u54C1\u306B\u306F\u3088\u304F\u767B\u5834\u3059\u308B\u304C\u3001\u73FE\u5B9F\u306B\u306F\u6280\u8853\u7684\u306A\u56F0\u96E3\u3092\u4F34\u3046\u305F\u30812022\u5E74\u73FE\u5728\u5B9F\u7528\u5316\u306F\u3055\u308C\u3066\u3044\u306A\u3044 \u3002"@ja ,
"Dalam fisika nuklir, fusi nuklir (reaksi termonuklir) adalah sebuah reaksi di mana dua inti atom bergabung membentuk satu atau lebih inti atom yang lebih besar dan partikel subatom (neutron atau proton). Perbedaan dalam massa antara reaktan dan produk dimanifestasikan sebagai pelepasan energi dalam jumlah besar. Perbedaan dalam massa ini muncul akibat perbedaan dalam energi ikatan inti atom antara sebelum dan setelah reaksi. Fusi nuklir adalah proses yang memberikan daya bagi bintang untuk bersinar. Proses fusi yang menghasilkan nukleus lebih ringan dari besi-56 atau secara umum tidak akan melepaskan sejumlah energi bersih. Elemen-elemen ini memiliki massa per nukleon terendah dan energi ikatan per nukleon tertinggi. Fusi elemen-elemen ringan akan melepas energi (eksotermis), sedangkan fusi yang menghasilkan inti lebih berat dari elemen ini, akan menghasilkan energi yang ditahan oleh nukleon yang dihasilkan. Kebalikannya ini benar untuk proses yang berkebalikan, fisi nuklir. Hal ini berarti untuk elemen ringan, seperti hidrogen dan secara umum lebih mudah fusi; sedangkan untuk elemen yang lebih berat, seperti uranium dan plutonium, lebih mudah fisi. Proses fusi membutuhkan energi yang besar untuk menggabungkan inti nuklir, bahkan elemen yang paling ringan, hidrogen. Tetapi fusi inti atom yang membentuk inti atom yang lebih berat dan neutron bebas, akan menghasilkan energi yang lebih besar lagi dari energi yang dibutuhkan untuk menggabungkan mereka\u2014sebuah yang dapat menciptakan reaksi yang terjadi sendirinya. Energi yang dilepas di banyak reaksi nuklir lebih besar dari reaksi kimia, karena yang mengelem kedua inti atom jauh lebih besar dari energi yang menahan elektron ke inti atom. Contoh, energi ionisasi yang diperoleh dari penambahan elektron ke hidrogen adalah elektronvolt\u2014lebih kecil satu per sejuta dari 17 MeV yang dilepas oleh reaksi D-T seperti gambar di samping."@in ,
"La fusi\u00F3 nuclear consisteix en una reacci\u00F3 en la qual dos nuclis at\u00F2mics (per exemple de deuteri) es converteixen en un nucli m\u00E9s pesant (en l'exemple heli), aquesta reacci\u00F3 va acompanyada de l'emissi\u00F3 de part\u00EDcules (en l'exemple del deuteri un neutr\u00F3). Aquestes reaccions poden produir una gran emissi\u00F3 d'energia, en forma de raigs gamma i d'energia cin\u00E8tica de les part\u00EDcules emeses. Aquesta emissi\u00F3 d'energia \u00E9s apreciable disminuci\u00F3 de massa per la famosa f\u00F3rmula d'Einstein E=mc\u00B2. A difer\u00E8ncia de la fissi\u00F3, que es basa a trencar un \u00E0tom molt pesant (d'urani o de plutoni, per exemple) i fer-ne apar\u00E8ixer de m\u00E9s lleugers (radi entre d'altres), la fusi\u00F3 consisteix a unir \u00E0toms lleugers i convertir-los en un de m\u00E9s pesant. Els residus radioactius resultants tenen un per\u00EDode de semidesintegraci\u00F3 extremadament curt en comparaci\u00F3 amb els de la fissi\u00F3. Aquests poden ser del voltant d'un dia. \u00C9s a dir, que en m\u00E9s o menys un dia, deixen de ser radioactius, o redueixen molt la seva perillositat, tot i que en el cas de l'urani aquest pot trigar m\u00E9s de 300.000 anys a deixar de ser radioactiu. La fusi\u00F3 nuclear no s'ha de confondre amb la fusi\u00F3 de nucli, que fa refer\u00E8ncia a l'accident en qu\u00E8 la part m\u00E9s interna (nucli) d'un reactor nuclear es fon com a resultat d'un sobreescalfament produ\u00EFt per una refrigeraci\u00F3 deficient."@ca ,
"Fusio nuklearra prozesu atomiko bat da, non bi nukleo edo gehiago batzen diren beste nukleo astunago bat sortzeko. Prozesu honekin energia kopuru handia igortzen edo xurgatzen da. Fusio nuklearra modu naturalean gertatzen da izarren barnean, eta artifizialki fusioko lehergailu termonuklearretan (H lehergailuan) eta fusio erreaktore esperimentaletan. Azken aplikazio horren bidez energia iturri honi erabilera zibila eman nahi zaio, elektrizitatea sortzeko, baina oraindik fase esperimentalean dago."@eu ,
"Nuclear fusion is a reaction in which two or more atomic nuclei are combined to form one or more different atomic nuclei and subatomic particles (neutrons or protons). The difference in mass between the reactants and products is manifested as either the release or absorption of energy. This difference in mass arises due to the difference in nuclear binding energy between the atomic nuclei before and after the reaction. Nuclear fusion is the process that powers active or main sequence stars and other high-magnitude stars, where large amounts of energy are released. A nuclear fusion process that produces atomic nuclei lighter than iron-56 or nickel-62 will generally release energy. These elements have a relatively small mass and a relatively large binding energy per nucleon. Fusion of nuclei lighter than these releases energy (an exothermic process), while the fusion of heavier nuclei results in energy retained by the product nucleons, and the resulting reaction is endothermic. The opposite is true for the reverse process, called nuclear fission. Nuclear fusion uses lighter elements, such as hydrogen and helium, which are in general more fusible; while the heavier elements, such as uranium, thorium and plutonium, are more fissionable. The extreme astrophysical event of a supernova can produce enough energy to fuse nuclei into elements heavier than iron."@en ,
"\u0422\u0435\u0440\u043C\u043E\u044F\u0301\u0434\u0435\u0440\u043D\u0430\u044F \u0440\u0435\u0430\u0301\u043A\u0446\u0438\u044F \u2014 \u0440\u0430\u0437\u043D\u043E\u0432\u0438\u0434\u043D\u043E\u0441\u0442\u044C \u044F\u0434\u0435\u0440\u043D\u043E\u0439 \u0440\u0435\u0430\u043A\u0446\u0438\u0438, \u043F\u0440\u0438 \u043A\u043E\u0442\u043E\u0440\u043E\u0439 \u043B\u0451\u0433\u043A\u0438\u0435 \u0430\u0442\u043E\u043C\u043D\u044B\u0435 \u044F\u0434\u0440\u0430 \u043E\u0431\u044A\u0435\u0434\u0438\u043D\u044F\u044E\u0442\u0441\u044F \u0432 \u0431\u043E\u043B\u0435\u0435 \u0442\u044F\u0436\u0451\u043B\u044B\u0435 \u0437\u0430 \u0441\u0447\u0451\u0442 \u043A\u0438\u043D\u0435\u0442\u0438\u0447\u0435\u0441\u043A\u043E\u0439 \u044D\u043D\u0435\u0440\u0433\u0438\u0438 \u0438\u0445 \u0442\u0435\u043F\u043B\u043E\u0432\u043E\u0433\u043E \u0434\u0432\u0438\u0436\u0435\u043D\u0438\u044F."@ru ,
"In chimica nucleare e in fisica nucleare, la fusione nucleare \u00E8 una reazione nucleare nella quale i nuclei di due o pi\u00F9 atomi si uniscono tra loro formando il nucleo di un nuovo elemento chimico. Perch\u00E9 la fusione sia possibile i nuclei devono essere avvicinati tra loro, impiegando una grande energia per superare la repulsione elettromagnetica. La fusione degli elementi fino ai numeri atomici 26 e 28 (ferro e nichel) \u00E8 una reazione esotermica, cio\u00E8 emette energia poich\u00E9 il nucleo prodotto dalla reazione ha massa minore della somma delle masse dei nuclei reagenti. Per gli atomi con numeri atomici superiori la reazione invece \u00E8 endotermica, cio\u00E8 assorbe energia. Alcune reazioni (in primo luogo quelle con una soglia di energia pi\u00F9 bassa, come la fusione di deuterio e trizio) determinano il rilascio di uno o pi\u00F9 neutroni liberi; questo crea, nella prospettiva dello sfruttamento come fonte di energia, alcuni importanti problemi tecnologici legati alla attivazione neutronica e alla schermatura. Il processo di fusione di nuclei atomici \u00E8 il meccanismo alla base delle stelle, rendendo possibile l'emissione di luce e il mantenimento costante delle loro dimensioni impedendone il collasso gravitazionale. La fusione \u00E8 stata per la prima volta prodotta artificialmente negli anni Cinquanta per amplificare la potenza di una bomba atomica: questo tipo di ordigni \u00E8 stato chiamato bomba H. A partire dagli anni Sessanta, sono stati eseguiti molti esperimenti per sfruttare l'energia prodotta dalla fusione, in primis per produrre energia elettrica. I reattori nucleari a fusione sono ancora in corso di progettazione e di costruzione. Si crede che il lavoro venga concluso circa intorno al 2060. Il giorno 13 dicembre 2022 il Dipartimento dell'energia degli Stati Uniti d'America ha annunciato la prima fusione nucleare la cui reazione ha prodotto pi\u00F9 energia di quanta utilizzata per produrne."@it ,
"Fuzio a\u016D nuklea kunfandi\u011Do (angle nuclear fusion), estas kuni\u011Do de subatomaj partikloj a\u016D nukleoj (atomkernoj) por formi pli grandajn nukleojn. Kiam fuzio okazas al nukleoj pli malgrandaj ol nukleo de fero, la maso iomete malpligrandi\u011Das dum la reakcio, kaj konverti\u011Das al elradianta energio."@eo ,
"La fusion nucl\u00E9aire (ou thermonucl\u00E9aire) est une r\u00E9action nucl\u00E9aire dans laquelle deux noyaux atomiques s\u2019assemblent pour former un noyau plus lourd. Cette r\u00E9action est \u00E0 l\u2019\u0153uvre de mani\u00E8re naturelle dans le Soleil et la plupart des \u00E9toiles de l'Univers, dans lesquelles sont cr\u00E9\u00E9s tous les \u00E9l\u00E9ments chimiques autres que l'hydrog\u00E8ne et la majeure partie de l'h\u00E9lium. Elle est, avec la fission nucl\u00E9aire, l\u2019un des deux principaux types de r\u00E9actions nucl\u00E9aires appliqu\u00E9es. La fusion nucl\u00E9aire d\u00E9gage une quantit\u00E9 d\u2019\u00E9nergie colossale par unit\u00E9 de masse, provenant de l\u2019attraction entre les nucl\u00E9ons due \u00E0 l\u2019interaction forte (voir \u00E9nergie de liaison nucl\u00E9aire). La masse du ou des produits d'une r\u00E9action de fusion \u00E9tant inf\u00E9rieure \u00E0 la somme des masses des noyaux fusionn\u00E9s, la diff\u00E9rence est transform\u00E9e en \u00E9nergie cin\u00E9tique (puis en chaleur) selon la formule d'Einstein E = mc2. La fusion nucl\u00E9aire est utilis\u00E9e dans les bombes H et, de fa\u00E7on plus anecdotique, dans les g\u00E9n\u00E9rateurs de neutrons. Elle pourrait \u00EAtre utilis\u00E9e pour la production d'\u00E9lectricit\u00E9, pour laquelle elle pr\u00E9sente deux int\u00E9r\u00EAts majeurs : \n* la disponibilit\u00E9 de son \u00AB combustible \u00BB : \n* le deut\u00E9rium, pr\u00E9sent \u00E0 l'\u00E9tat naturel en quantit\u00E9s importantes dans les oc\u00E9ans, \n* le tritium (pour la r\u00E9action de fusion \u00AB deut\u00E9rium + tritium \u00BB), qui peut \u00EAtre produit par bombardement neutronique du lithium 6. Les r\u00E9serves mondiales en minerai de lithium suffiraient th\u00E9oriquement \u00E0 garantir plus d'un million d'ann\u00E9es de fonctionnement ; \n* son caract\u00E8re essentiellement \u00AB propre \u00BB : les produits de la fusion eux-m\u00EAmes (principalement de l\u2019h\u00E9lium 4) ne sont pas radioactifs. Les d\u00E9chets potentiels se limitent, lorsque la r\u00E9action utilis\u00E9e \u00E9met des neutrons rapides, aux mat\u00E9riaux environnants, qui peuvent capturer ces neutrons et devenir \u00E0 leur tour des isotopes radioactifs. En d\u00E9pit de travaux de recherche r\u00E9alis\u00E9s dans le monde entier depuis les ann\u00E9es 1950, aucune application industrielle de la fusion \u00E0 la production d\u2019\u00E9nergie n\u2019a encore abouti. Les ing\u00E9nieurs se heurtent \u00E0 la difficult\u00E9 de cr\u00E9er et de maintenir une temp\u00E9rature de plusieurs millions de degr\u00E9s dans un espace confin\u00E9. La fusion nucl\u00E9aire n'a rien \u00E0 voir avec la fusion du c\u0153ur d'un r\u00E9acteur nucl\u00E9aire, qui est un accident nucl\u00E9aire particuli\u00E8rement redoutable."@fr ,
"Als Kernfusion werden Kernreaktionen bezeichnet, bei denen je zwei Atomkerne zu einem neuen Kern verschmelzen. Kernfusionsreaktionen sind die Ursache daf\u00FCr, dass die Sonne und alle leuchtenden Sterne Energie abstrahlen. Von entscheidender Bedeutung f\u00FCr das Zustandekommen einer Fusion ist der Wirkungsquerschnitt, das Ma\u00DF f\u00FCr die Wahrscheinlichkeit, dass zusammensto\u00DFende Kerne miteinander reagieren. Ausreichend gro\u00DF ist der Wirkungsquerschnitt meist nur dann, wenn die beiden Kerne mit hoher Energie aufeinander prallen. Diese ist n\u00F6tig, um die Coulombbarriere, die elektrische Absto\u00DFung zwischen den positiv geladenen Kernen, zu \u00FCberwinden oder ihr schmales Maximum zu durchtunneln. Jenseits der Barriere, bei einem Abstand von nur noch etwa 10\u221215 m, \u00FCberwiegt die Anziehung durch die starke Wechselwirkung und die Kerne verschmelzen miteinander. Fusionsreaktionen k\u00F6nnen exotherm (Energie abgebend) oder endotherm (Energie aufnehmend) sein. Exotherme Fusionsreaktionen k\u00F6nnen die hohen Temperaturen aufrechterhalten, die n\u00F6tig sind, damit die thermische Energie zu weiteren Fusionsreaktionen f\u00FChren kann. Solche thermonuklearen Prozesse laufen in Sternen und Fusionsbomben unter extremem Druck ab. Im Gegensatz zur Kernspaltung ist eine Kettenreaktion mit Fusionsreaktionen nicht m\u00F6glich. Die oben abgebildete Fusionsreaktion als thermonuklearer Vorgang soll in Zukunft der Stromerzeugung in Kernfusionsreaktoren dienen: Kerne von Deuterium (2H) und Tritium (3H) verschmelzen zu einem Heliumkern (4He) unter Freisetzung eines Neutrons (n) sowie von Energie (3,5 MeV + 14,1 MeV). In der Abbildung darunter ist die Bindungsenergie pro Nukleon der Nuklide dargestellt. Energie wird frei bei Reaktionen in aufsteigender Richtung der Kurve bzw. wird ben\u00F6tigt bei abfallender Richtung. Die Fusion von Wasserstoff (H) zu Helium-4 setzt besonders viel Energie frei."@de ,
"\u03A0\u03C5\u03C1\u03B7\u03BD\u03B9\u03BA\u03AE \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7 (\u03C3\u03C5\u03BD + \u03C4\u03AE\u03BE\u03B7) \u03BF\u03BD\u03BF\u03BC\u03AC\u03B6\u03B5\u03C4\u03B1\u03B9 \u03B7 \u03C3\u03C5\u03BD\u03AD\u03BD\u03C9\u03C3\u03B7 \u03B5\u03BB\u03B1\u03C6\u03C1\u03CE\u03BD \u03C0\u03C5\u03C1\u03AE\u03BD\u03C9\u03BD \u03C3\u03B5 \u03B2\u03B1\u03C1\u03CD\u03C4\u03B5\u03C1\u03BF\u03C5\u03C2 \u03BC\u03B5 \u03C4\u03B1\u03C5\u03C4\u03CC\u03C7\u03C1\u03BF\u03BD\u03B7 \u03B1\u03C0\u03B5\u03BB\u03B5\u03C5\u03B8\u03AD\u03C1\u03C9\u03C3\u03B7 \u03B5\u03BD\u03AD\u03C1\u03B3\u03B5\u03B9\u03B1\u03C2, \u03B4\u03B7\u03BB\u03B1\u03B4\u03AE \u03C0\u03C1\u03CC\u03BA\u03B5\u03B9\u03C4\u03B1\u03B9 \u03B3\u03B9\u03B1 \u03B5\u03BE\u03CE\u03B8\u03B5\u03C1\u03BC\u03B7 \u03B1\u03BD\u03C4\u03AF\u03B4\u03C1\u03B1\u03C3\u03B7. \u0392\u03AD\u03B2\u03B1\u03B9\u03B1 \u03B3\u03B9\u03B1 \u03BD\u03B1 \u03B8\u03B5\u03C9\u03C1\u03B7\u03B8\u03B5\u03AF \u03B5\u03BE\u03CE\u03B8\u03B5\u03C1\u03BC\u03B7 \u03B1\u03BD\u03B1\u03C6\u03B5\u03C1\u03CC\u03BC\u03B1\u03C3\u03C4\u03B5 \u03C3\u03B5 \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7 \u03B5\u03BB\u03B1\u03C6\u03C1\u03CE\u03BD \u03C0\u03C5\u03C1\u03AE\u03BD\u03C9\u03BD \u03BC\u03AD\u03C7\u03C1\u03B9 \u03C4\u03BF \u03C3\u03AF\u03B4\u03B7\u03C1\u03BF-56 \u03AE \u03BD\u03B9\u03BA\u03AD\u03BB\u03B9\u03BF-62. \u039A\u03B1\u03C4\u03AC \u03C4\u03B7 \u03C3\u03CD\u03BD\u03C4\u03B7\u03BE\u03B7 \u03B2\u03B1\u03C1\u03CD\u03C4\u03B5\u03C1\u03C9\u03BD \u03C0\u03C5\u03C1\u03AE\u03BD\u03C9\u03BD \u03B1\u03C0\u03CC \u03B1\u03C5\u03C4\u03BF\u03CD\u03C2 \u03C5\u03C0\u03AC\u03C1\u03C7\u03B5\u03B9 \u03B5\u03BD\u03B5\u03C1\u03B3\u03B5\u03B9\u03B1\u03BA\u03CC \u03AD\u03BB\u03BB\u03B5\u03B9\u03BC\u03BC\u03B1 \u03BA\u03B1\u03B9 \u03B7 \u03B1\u03BD\u03C4\u03AF\u03B4\u03C1\u03B1\u03C3\u03B7 \u03B3\u03AF\u03BD\u03B5\u03C4\u03B1\u03B9 \u03B5\u03BD\u03B4\u03CC\u03B8\u03B5\u03C1\u03BC\u03B7."@el ,
"Nuair a nascann dh\u00E1 n\u00FAicl\u00E9as bheaga le ch\u00E9ile chun n\u00FAicl\u00E9as n\u00EDos m\u00F3 a dh\u00E9anamh,sin comhle\u00E1 n\u00FAicl\u00E9ach. Scaoiltear fuinneamh n\u00FAicl\u00E9ach amach as n\u00FAicl\u00E9as nuair a chomhle\u00E1itear dh\u00E1 n\u00FAicl\u00E9\u00F3n n\u00F3 dh\u00E1 n\u00FAicl\u00E9as bheaga (mar shampla n\u00FAicl\u00E9as de dheoit\u00E9iriaim is n\u00FAicl\u00E9as de thritiam, dh\u00E1 iseat\u00F3p hidrigine) le ch\u00E9ile chun n\u00FAicl\u00E9as n\u00EDos m\u00F3 a chruth\u00FA. Athr\u00FA maise chuig fuinneamh is bun leis an gcruth\u00FA fuinnimh seo. Chun comhle\u00E1 a chur chun cinn, n\u00ED m\u00F3r na n\u00FAicl\u00E9is bheaga at\u00E1 araon luchtaithe go dearfach a bhr\u00FA chomh gar sin d\u00E1 ch\u00E9ile go s\u00E1ra\u00EDtear a gcomh\u00E9aradh. Imoibri\u00FA comhle\u00E1ite is bun le teas na Gr\u00E9ine is na r\u00E9alta\u00ED eile, agus an rada\u00EDocht go l\u00E9ir a asta\u00EDonn siad. Crutha\u00EDtear teocht ard go leor chun gur f\u00E9idir an comhle\u00E1 a dh\u00E9anamh i bpl\u00E9asc\u00E1n n\u00FAicl\u00E9ach eamhnaithe. Mar sin, sna H-bhuama\u00ED, is amhlaidh a bh\u00EDonn pl\u00E9asc bheag eamhnaithe a chrutha\u00EDonn an ardteocht chun pl\u00E9asc comhle\u00E1ite a mhadhmadh. I dt\u00EDortha ar fud an domhain, t\u00E1thar ag iarraidh an t-imoibri\u00FA seo a chur ar si\u00FAl ar bhonn lean\u00FAnach sti\u00FArtha chun an fuinneamh a fh\u00E1il uaidh agus cumhacht leictreach a ghini\u00FAint uaidh sin. N\u00ED th\u00E9ann an t-imoibri\u00FA ar aghaidh oiread ar fi\u00FA tr\u00E1cht air ach nuair a bh\u00EDonn teocht is br\u00FA f\u00EDorard i bhfeidhm. N\u00EDl s\u00E9 \u00E9asca n\u00E1 saor na coinn\u00EDollacha seo a chomhl\u00EDonadh."@ga ,
"\u6838\u805A\u53D8\uFF08\u53F0\u6E7E\u7A31\u70BA\u6838\u878D\u5408\uFF09\uFF0C\uFF08\u82F1\u8A9E\uFF1ANuclear fusion\u3001 \u5FB7\u8A9E\uFF1AKernfusion\uFF09\u53C8\u7A31\u878D\u5408\u53CD\u61C9\uFF0C\u662F\u6307\u5C06\u4E24\u4E2A\u8F83\u8F7B\u7684\u6838\u7ED3\u5408\u800C\u5F62\u6210\u4E00\u4E2A\u8F83\u91CD\u7684\u6838\u548C\u4E00\u4E2A\u6975\u8F7B\u7684\u6838\uFF08\u6216\u7C92\u5B50\uFF09\u7684\u4E00\u79CD\u6838\u53CD\u5E94\u5F62\u5F0F\u3002\u5728\u6B64\u8FC7\u7A0B\u4E2D\uFF0C\u7269\u8D28\u4E26\u6CA1\u6709\u5B88\u6052\uFF0C\u56E0\u4E3A\u6709\u4E00\u90E8\u5206\u6B63\u5728\u805A\u53D8\u7684\u539F\u5B50\u6838\u7684\u7269\u8D28\u88AB\u8F6C\u5316\u4E3A\u5149\u5B50\uFF08\u80FD\u91CF\uFF09\u3002\u6838\u805A\u53D8\u662F\u7ED9\u6D3B\u8DC3\u7684\u6216\u201C\u4E3B\u5E8F\u7684\u201D\u6046\u661F\u63D0\u4F9B\u80FD\u91CF\u7684\u8FC7\u7A0B\u3002 \u4E24\u4E2A\u8F83\u8F7B\u7684\u6838\u5728\u878D\u5408\u8FC7\u7A0B\u4E2D\u4EA7\u751F\u8D28\u91CF\u8017\u640D\u800C\u91CA\u653E\u51FA\u5DE8\u5927\u7684\u80FD\u91CF\uFF0C\u4E24\u4E2A\u8F7B\u6838\u5728\u53D1\u751F\u805A\u53D8\u65F6\u867D\u7136\u56E0\u5B83\u4EEC\u90FD\u5E26\u6B63\u7535\u8377\u800C\u5F7C\u6B64\u6392\u65A5\uFF0C\u7136\u800C\u4E24\u4E2A\u80FD\u91CF\u8DB3\u591F\u9AD8\u7684\u6838\u8FCE\u9762\u76F8\u9047\uFF0C\u5B83\u4EEC\u5C31\u80FD\u76F8\u5F53\u7D27\u5BC6\u5730\u805A\u96C6\u5728\u4E00\u8D77\uFF0C\u4EE5\u81F4\u6838\u529B\u80FD\u591F\u514B\u670D\u5E93\u4ED1\u65A5\u529B\u800C\u53D1\u751F\u6838\u53CD\u5E94\uFF0C\u8FD9\u4E2A\u53CD\u5E94\u53EB\u505A\u6838\u805A\u53D8\u3002 \u8209\u4F8B\uFF1A\u4E24\u4E2A\u8CEA\u91CF\u5C0F\u7684\u539F\u5B50\uFF0C\u6BD4\u65B9\u8AAA\u5169\u500B\u6C18\u539F\u5B50\uFF0C\u5728\u4E00\u5B9A\u6761\u4EF6\u4E0B\uFF08\u5982\u8D85\u9AD8\u6E29\u548C\u9AD8\u538B\uFF09\uFF0C\u6703\u53D1\u751F\u539F\u5B50\u6838\u4E92\u76F8\u805A\u5408\u4F5C\u7528\uFF0C\u751F\u6210\u4E2D\u5B50\u548C\u6C26-3\uFF0C\u5E76\u4F34\u968F\u7740\u5DE8\u5927\u7684\u80FD\u91CF\u91CA\u653E\u3002 \u539F\u5B50\u6838\u4E2D\u8574\u85CF\u5DE8\u5927\u7684\u80FD\u91CF\u3002\u6839\u636E\u8D28\u80FD\u65B9\u7A0BE=mc2\uFF0C\u539F\u5B50\u6838\u4E4B\u6DE8\u8D28\u91CF\u53D8\u5316\uFF08\u53CD\u61C9\u7269\u8207\u751F\u6210\u7269\u4E4B\u8CEA\u91CF\u5DEE\uFF09\u9020\u6210\u80FD\u91CF\u7684\u91CA\u653E\u3002\u5982\u679C\u662F\u7531\u91CD\u7684\u539F\u5B50\u6838\u53D8\u5316\u4E3A\u8F7B\u7684\u539F\u5B50\u6838\uFF0C\u7A31\u70BA\u6838\u88C2\u53D8\uFF0C\u5982\u539F\u5B50\u5F39\u7206\u70B8\uFF1B\u5982\u679C\u662F\u7531\u8F03\u8F7B\u7684\u539F\u5B50\u6838\u53D8\u5316\u4E3A\u8F03\u91CD\u7684\u539F\u5B50\u6838\uFF0C\u7A31\u70BA\u6838\u805A\u53D8\u3002\u4E00\u822C\u4F86\u8AAA\uFF0C\u9019\u7A2E\u6838\u53CD\u5E94\u6703\u7D42\u6B62\u65BC\u9435\uFF0C\u56E0\u70BA\u5176\u539F\u5B50\u6838\u6700\u70BA\u7A69\u5B9A\u3002 1920\u5E74\uFF0C\u4E9A\u745F\u00B7\u7231\u4E01\u987F\u63D0\u51FA\u6C2B\u6C26\u805A\u8B8A\u53EF\u80FD\u662F\u6046\u661F\u80FD\u91CF\u7684\u4E3B\u8981\u4F86\u6E90\u3002\u5728\u6B27\u5185\u65AF\u7279\u00B7\u5362\u745F\u798F\u7684\u6838\u5B17\u53D8\u5BE6\u9A57\u57FA\u790E\u4E0A\uFF0C\u9A6C\u514B\u00B7\u5965\u5229\u82AC\u7279\u65BC1932\u5E74\u5B8C\u6210\u4E86\u6C2B\u540C\u4F4D\u7D20\u7684\u5BE6\u9A57\u5BA4\u805A\u8B8A\u30021930\u5E74\u4EE3\uFF0C\u6C49\u65AF\u00B7\u8D1D\u7279\u63D0\u51FA\u4E86\u6046\u661F\u6838\u805A\u8B8A\u4E3B\u5FAA\u74B0\u7684\u7406\u8AD6\u30021940\u5E74\u4EE3\u521D\uFF0C\u4F5C\u70BA\u66FC\u54C8\u9813\u8A08\u5283\u7684\u4E00\u90E8\u5206\uFF0C\u958B\u59CB\u7814\u7A76\u7528\u65BC\u8ECD\u4E8B\u76EE\u7684\u7684\u6838\u805A\u8B8A\u30021951\u5E74\uFF0C\u5728\u6838\u8A66\u9A57\u4E2D\u5B8C\u6210\u4E86\u6838\u805A\u8B8A\u30021952\u5E7411\u67081\u65E5\uFF0C\u5728\u5E38\u6625\u85E4\u9EA5\u514B\u6C2B\u5F48\u8A66\u9A57\u4E2D\u9996\u6B21\u9032\u884C\u4E86\u5927\u898F\u6A21\u6838\u805A\u8B8A\u3002 \u6700\u65E9\u7684\u4EBA\u5DE5\u6838\u878D\u5408\u6280\u8853\u5728\u6C2B\u5F48\u4E0A\u5F97\u5230\u4F53\u73B0\u30021950\u5E74\u4EE3\uFF0C\u4EBA\u7C7B\u5F00\u59CB\u7814\u7A76\u7528\u4E8E\u6C11\u7528\u76EE\u7684\u7684\u53D7\u63A7\u70ED\u6838\u805A\u53D8\u3002"@zh ;
dbo:wikiPageWikiLink dbr:Free_neutron ,
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dbr:Norman_Rostoker ,
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dbr:University_of_Oxford_Press ,
,
dbr:Austrian_Institute_of_Ecology ,
dbr:Nuclear_fusion_reactions ,
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