{ "format" : "linked-data-api", "version" : "0.2", "result" : {"_about" : "https://vocabs.ardc.edu.au/repository/api/lda/aas/the-unified-astronomy-thesaurus/5-0-0/resource.text?uri=http://astrothesaurus.org/uat/195", "definition" : "https://vocabs.ardc.edu.au/repository/api/lda/aas/the-unified-astronomy-thesaurus/5-0-0/resource.text?uri=http://astrothesaurus.org/uat/195", "extendedMetadataVersion" : "https://vocabs.ardc.edu.au/repository/api/lda/aas/the-unified-astronomy-thesaurus/5-0-0/resource.text?_metadata=all&uri=http://astrothesaurus.org/uat/195", "primaryTopic" : {"_about" : "http://astrothesaurus.org/uat/195", "broader" : [{"_about" : "http://astrothesaurus.org/uat/1131", "narrower" : ["http://astrothesaurus.org/uat/195"]} ], "contributor" : "http://editor.vocabs.ands.org.au/user/AAS_Frey.Katie_Admin", "dctermsModified" : "Tue, 24 Nov 2020 19:33:11 GMT+0000", "definition" : "The stage in the evolution of a star after helium burning when the core of the star consists mainly of carbon and oxygen. In stars of mass greater than about 8 solar masses, whose cores reach a temperature above 5 x 10^8 K and density above 3 x 10^9 kg m^-3, carbon burning can begin via reactions such as the following: 12C + 12C → 20Ne + 4He or 12C + 12C → 23Na + p or 12C + 12C → 23Mg + n. The time-scale for this phase of nucleosynthesis is of order of five hundred years.", "prefLabel" : {"_value" : "Carbon burning", "_lang" : "en"} , "type" : ["http://www.w3.org/2000/01/rdf-schema#Resource", "http://www.w3.org/2004/02/skos/core#Concept"]} , "type" : ["http://purl.org/linked-data/api/vocab#ItemEndpoint", "http://purl.org/linked-data/api/vocab#Page"]} }