Stellar fusion doesn’t stop at helium

Abstract

In the feature article “Ultracompact Binary Stars” by Gijs Nelemans (Physics Today, July 2006, page 26), box 1 all but declares that stars less than 8 solar masses fuse hydrogen into helium, and that’s it. Not so: Stars with more than about half a solar mass will go on to fuse helium into carbon and oxygen as well. In fact, the accepted picture of an entire class of stars, RR Lyrae variables, consists of stars less massive than the Sun that burn helium in their cores and hydrogen in a shell.Plenty of readable descriptions of this are available, from basic but clear, 1 1. V. Trimble, Visit to a Small Universe, American Institute of Physics, New York (1992), p. 121. to intermediate, 2 2. W. K. Rose, Advanced Stellar Astrophysics, Cambridge U. Press, New York (1998), p. 19; M. Harwit, Astrophysical Concepts, 2nd ed., Springer, New York (1988), p. 15. to more advanced. 3 3. R. Kippenhahn, A. Weigert, Stellar Structure and Evolution, Springer, New York (1990), p. 308. https://doi.org/10.1007/978-3-642-61523-8_32 REFERENCESSection:ChooseTop of pageREFERENCES <<1. V. Trimble, Visit to a Small Universe, American Institute of Physics, New York (1992), p. 121. Google Scholar2. W. K. Rose, Advanced Stellar Astrophysics, Cambridge U. Press, New York (1998), p. 19; Google ScholarCrossref M. Harwit, Astrophysical Concepts, 2nd ed., Springer, New York (1988), p. 15. , Google ScholarCrossref3. R. Kippenhahn, A. Weigert, Stellar Structure and Evolution, Springer, New York (1990), p. 308. https://doi.org/10.1007/978-3-642-61523-8_32 , Google ScholarCrossref© 2007 American Institute of Physics.