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Stellar evolution

Stellar evolution is the process by which a star changes over the course of time. Depending on the mass of the star, its lifetime can range from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the current age of the universe.

Star formation, Stellar remnants & Mature stars

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Overview

Star formation

Mature stars

Stellar remnants

Models

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Stellar evolution

Nodes147
Edges146
Triples62
Avg. degree1.99
Density0.013605
Components1

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Stellar evolution

Top relations

related to References · 21
Stellar evolution → An Introduction, Andrew, Cambridge University Press, Carl, Dina, Evolution, Hansen, ISBN, Kawaler, Norton, Nucleosynthesis, Prialnik, Ryan, Sean, Springer-Verlag, Stellar, Stellar Structure, Steven, Theory, Trimble
related to External links · 14
Stellar evolution → BBC Radio, Experiments, In Our Time, Janna Levin, Life, Mar, Modules, Paul Murdin, Phil Charles, Stars, Stellar, Stellar Astrophysics, Stellar ModelsMESA, The Life
related to Protostar · 10
Stellar evolution → As, Continuous, Dense, Filamentary, Further, In, Mass, Stellar, Sun, Typical
related to Models · 5
Stellar evolution → Accurate, Extensive, Hertzsprung, Russell, The
is a · 1
Stellar evolution → process by which a star changes over the course of time

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Important terminology

stars star core fusion mass helium hydrogen carbon stellar massive energy white supernova collapse fuse evolution sun dwarf enough red

Entity relationships Subject–Predicate–Object triples

SubjectPredicateObjectConfidenceSrc
Stellar evolutionis aprocess by which a star changes over the course of time0.90text
metallicityinstance ofThe morphology of the horizontal branch depends on parameters0.80text
ageinstance ofThe morphology of the horizontal branch depends on parameters0.80text
and helium contentinstance ofThe morphology of the horizontal branch depends on parameters0.80text
but the exact details are still being modelled.Asymptotic-giant-branch phaseAfter a star has consumed the helium at the coreinstance ofThe morphology of the horizontal branch depends on parameters0.80text
hydrogeninstance ofThe morphology of the horizontal branch depends on parameters0.80text
helium fusion continues in shells around a hot core of carboninstance ofThe morphology of the horizontal branch depends on parameters0.80text
oxygeninstance ofThe morphology of the horizontal branch depends on parameters0.80text
metallicityinstance ofand these stars will eventually leave an oxygen-neon-magnesium white dwarf.The exact mass limit for full carbon burning depends on several factors0.80text
the detailed mass lost on the asymptotic giant branchinstance ofand these stars will eventually leave an oxygen-neon-magnesium white dwarf.The exact mass limit for full carbon burning depends on several factors0.80text
but is approximately 8instance ofand these stars will eventually leave an oxygen-neon-magnesium white dwarf.The exact mass limit for full carbon burning depends on several factors0.80text
but the exact details are still being modelledinstance ofThe morphology of the horizontal branch depends on parameters0.80text

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