helium burning
(helium fusion)
(fusion reaction starting with helium)
Helium burning is fusion of helium nuclei, specifically,
the triple alpha process, which takes place in early
stars, producing carbon and some and oxygen. In a
sufficiently-massive star, helium burning occurs within the
stellar core subsequent to its RGB (red giant branch)
phase, comprising a further phase termed the horizontal branch (or for some
types of stars, the red clump).
When the carbon and oxygen have sunk to the center and helium burning
throughout the core has ceased,
a helium-burning shell can form surrounding
the core. In sufficiently-massive stars, additional types of fusion
begin within and surrounding the core as the density and temperature
increase. The above is the normal course of helium burning as part of
stellar evolution, but there are some more exotic situations,
particularly involving interacting binary stars. Helium burning
requires a temperature on the order of 5 × 108 K.
(fusion,nuclear,reaction,nucleosynthesis,atoms,helium)
Further reading:
https://en.wikipedia.org/wiki/Triple-alpha_process
https://en.wikipedia.org/wiki/Stellar_evolution#Massive_stars
https://en.wiktionary.org/wiki/helium_burning
https://dictionary.obspm.fr/index.php?formSearchTextfield=helium+burning&showAll=1
https://www.daviddarling.info/encyclopedia/H/helium_burning.html
https://web.phys.cmu.edu/~tiziana/stars/stars24.pdf
https://t2.lanl.gov/nis/tour/helium.html
http://www.people.vcu.edu/~rgowdy/astro/mod/048/t2/xmp.html
https://pages.uoregon.edu/jimbrau/astr122/Notes/Chapter20.html#helium
https://ui.adsabs.harvard.edu/abs/1972ApJ...176..681A/abstract
Referenced by pages:
asymptotic giant branch (AGB)
helium flash
horizontal branch (HB)
post-main-sequence star
red clump (RC)
red-giant branch (RGB)
Schönberg-Chandrasekhar limit
thermal pulse (TP)
triple alpha process
Type Ia supernova problem
Index