Editing Helium flash (section)

==Subflashes==
Subflashes are pulsational instabilities that occur after the main helium flash. They are driven by stars that do not have good convective or radiative boundaries.<ref name=":0">{{Cite journal |last1=Battich |first1=Tiara |last2=Bertolami |first2=Marcelo M. Miller |last3=Córsico |first3=Alejandro H. |last4=Althaus |first4=Leandro G. |date=2018-06-01 |title=Pulsational instabilities driven by the ∈ mechanism in hot pre-horizontal branch stars - I. The hot-flasher scenario |url=https://www.aanda.org/articles/aa/full_html/2018/06/aa31463-17/aa31463-17.html |journal=Astronomy & Astrophysics |language=en |volume=614 |pages=A136 |doi=10.1051/0004-6361/201731463 |arxiv=1801.07287 |bibcode=2018A&A...614A.136B |issn=0004-6361}}</ref> Subflashes can last several hours to days and can occur for many years with each subsequent flash generally being weaker.<ref name=":0" /> Subflashes can be detected by applying [[fourier transform]]s to the light curve data.<ref>{{Cite journal |last=Balona |first=Luis A. |date=2020-10-29 |title=The Hot Limit of Solar-like Oscillations From Kepler Photometry |journal=Frontiers in Astronomy and Space Sciences |language=English |volume=7 |page=85 |doi=10.3389/fspas.2020.529025 |doi-access=free |arxiv=2008.06299 |bibcode=2020FrASS...7...85B |issn=2296-987X}}</ref>