@prefix mdl: <http://data.loterre.fr/ark:/67375/MDL> .
@prefix skos: <http://www.w3.org/2004/02/skos/core#> .
@prefix dc: <http://purl.org/dc/terms/> .
@prefix xsd: <http://www.w3.org/2001/XMLSchema#> .

mdl:-ZF9QCN61-5
  skos:prefLabel "nucléosynthèse"@fr, "nucleosynthesis"@en ;
  a skos:Concept ;
  skos:narrower mdl:-W6TCPDK2-N .

mdl: a skos:ConceptScheme .
mdl:-CQ1N4XTP-9
  skos:prefLabel "nuclear fusion"@en, "fusion nucléaire"@fr ;
  a skos:Concept ;
  skos:narrower mdl:-W6TCPDK2-N .

mdl:-W6TCPDK2-N
  skos:prefLabel "combustion du carbone"@fr, "carbon burning"@en ;
  skos:hiddenLabel "carbon burnings"@en, "combustions des carbones"@fr, "Carbon burning"@en, "Combustion carbones"@fr, "Combustion carbone"@fr ;
  skos:broader mdl:-CQ1N4XTP-9, mdl:-ZF9QCN61-5 ;
  a skos:Concept ;
  skos:definition "The carbon-burning process or carbon fusion is a set of nuclear fusion reactions that take place in the cores of massive stars (at least 8 M⊙ at birth) that combines carbon into other elements. It requires high temperatures (> 5×10⁸ K or 50 keV) and densities (> 3×10⁹ kg/m3). These figures for temperature and density are only a guide. More massive stars burn their nuclear fuel more quickly, since they have to offset greater gravitational forces to stay in (approximate) hydrostatic equilibrium. That generally means higher temperatures, although lower densities, than for less massive stars. To get the right figures for a particular mass, and a particular stage of evolution, it is necessary to use a numerical stellar model computed with computer algorithms. Such models are continually being refined based on nuclear physics experiments (which measure nuclear reaction rates) and astronomical observations (which include direct observation of mass loss, detection of nuclear products from spectrum observations after convection zones develop from the surface to fusion-burning regions – known as dredge-up events – and so bring nuclear products to the surface, and many other observations relevant to models). (Wikipedia, The Free Encyclopedia, <a href=\"https://en.wikipedia.org/wiki/Carbon-burning_process\" target=\"_blank\">https://en.wikipedia.org/wiki/Carbon-burning_process</a>)"@en, "La fusion du carbone, souvent appelée (de façon plus ambigüe) \"combustion du carbone\", est un ensemble de réactions de fusion nucléaire intervenant dans les étoiles d'au moins cinq masses solaires à leur formation qui, en leur cœur, ont converti en carbone tous leurs éléments plus légers. Ces réactions se déroulent à une température d'au moins 600 MK alors que la masse volumique des gaz atteint 2×10⁸ kg/m3. (Wikipedia, L'Encylopédie Libre, <a href=\"https://fr.wikipedia.org/wiki/Fusion_du_carbone\" target=\"_blank\">https://fr.wikipedia.org/wiki/Fusion_du_carbone</a>)"@fr ;
  skos:exactMatch <https://en.wikipedia.org/wiki/Carbon-burning_process>, <https://fr.wikipedia.org/wiki/Fusion_du_carbone>, <http://astrothesaurus.org/uat/195> ;
  skos:inScheme mdl: ;
  dc:modified "2022-10-14"^^xsd:date .