Main sequence: Difference between revisions

Revision as of 23:16, 24 October 2023

Revision as of 23:16, 24 October 2023

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The observed upper limit for a main-sequence star is 120–200 {{solar mass}}.<ref name=apj620_1/> The theoretical explanation for this limit is that stars above this mass can not radiate energy fast enough to remain stable, so any additional mass will be ejected in a series of pulsations until the star reaches a stable limit.<ref name=apj162/> The lower limit for sustained proton-proton nuclear fusion is about 0.08 {{solar mass}} or 80 times the mass of [[Jupiter]].<ref name=hannu/> Below this threshold are sub-stellar objects that can not sustain hydrogen fusion, known as [[brown dwarf]]s.<ref name=apj406_1/>

=='''''Structure'''''==

{{Main|Stellar structure}}

[[File:Solar internal structure.svg|right|upright=1.0|thumb|This diagram shows a cross-section of a Sun-like star, showing the internal structure.]]