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Higher mass red supergiants blow away their outer atmospheres and evolve back to blue supergiants, and possibly onwards to Wolf–Rayet stars.<ref name=origlia>{{Cite journal | last1 = Origlia | first1 = L. | last2 = Goldader | first2 = J. D. | last3 = Leitherer | first3 = C. | last4 = Schaerer | first4 = D. | last5 = Oliva | first5 = E. | title = Evolutionary Synthesis Modeling of Red Supergiant Features in the Near‐Infrared | doi = 10.1086/306937 | journal = The Astrophysical Journal | volume = 514 | issue = 1 | pages = 96–108 | year = 1999 | pmid = | pmc = |arxiv = astro-ph/9810017 |bibcode = 1999ApJ...514...96O }}</ref><ref name=lmcysg>{{Cite journal|arxiv=1202.4225|author1=Neugent|author2=Philip Massey|author3=Brian Skiff|author4=Georges Meynet|title=Yellow and Red Supergiants in the Large Magellanic Cloud|journal=The Astrophysical Journal|volume=749|issue=2|pages=177|date=2012|doi=10.1088/0004-637X/749/2/177|bibcode = 2012ApJ...749..177N }}</ref> Depending on the exact mass and composition of a red supergiant, it can execute a number of blue loops before either exploding as a [[type II supernova]] or finally dumping enough of its outer layers to become a blue supergiant again, less luminous than the first time but more unstable.<ref name=rotating>{{Cite journal | last1 = Maeder | first1 = A. | last2 = Meynet | first2 = G. | doi = 10.1051/0004-6361:20010596 | title = Stellar evolution with rotation. VII | journal = Astronomy and Astrophysics | volume = 373 | issue = 2 | pages = 555–571 | year = 2001 | pmid = | pmc = |arxiv = astro-ph/0105051 |bibcode = 2001A&A...373..555M }}</ref> If such a star can pass through the yellow evolutionary void it is expected that it becomes one of the lower luminosity LBVs.<ref name=stothers>{{Cite journal | last1 = Stothers | first1 = R. B. | last2 = Chin | first2 = C. W. | doi = 10.1086/322438 | title = Yellow Hypergiants as Dynamically Unstable Post–Red Supergiant Stars | journal = The Astrophysical Journal | volume = 560 | issue = 2 | pages = 934 | year = 2001 | pmid = | pmc = |bibcode = 2001ApJ...560..934S }}</ref>

It is not clear whether more massive blue supergiants can lose enough mass to evolve safely into old age as a Wolf Rayet star and finally a white dwarf, or they reach the Wolf Rayet stage and explode as [[supernovae]], or they explode as supernovae while blue supergiants.

Supernova progenitors are most commonly red supergiants and it was believed that only red supergiants could explode as supernovae. [[SN 1987A]], however, forced astronomers to re-examine this theory, as its progenitor, [[Sanduleak -69° 202]], was a B3 blue supergiant.<ref>{{Cite book | last1 = Smith | first1 = N. | last2 = Immler | first2 = S. | last3 = Weiler | first3 = K. | doi = 10.1063/1.2803557 | chapter = Galactic Twins of the Nebula Around SN 1987A: Hints that LBVs may be supernova progenitors | title = AIP Conference Proceedings | journal = Aip Conf.proc | volume = 937 | pages = 163–170 | year = 2007 | pmid = | pmc = |arxiv = 0705.3066 }}</ref> Now it is known from observation that almost any class of evolved high-mass star, including blue and yellow supergiants, can explode as a supernova although theory still struggles to explain how in detail.<ref name=galyam>{{Cite journal | last1 = Gal-Yam | first1 = A. | last2 = Leonard | first2 = D. C. | doi = 10.1038/nature07934 | title = A Massive Hypergiant Star as the Progenitor of the Supernova SN 2005gl | journal = Nature | volume = 458 | issue = 7240 | pages = 865–867 | year = 2009 | pmid = 19305392 | url = http://hubblesite.org/pubinfo/pdf/2009/13/pdf.pdf | bibcode = 2009Natur.458..865G | access-date = 2015-08-28 | archive-url = https://web.archive.org/web/20160303224705/http://hubblesite.org/pubinfo/pdf/2009/13/pdf.pdf | archive-date = 2016-03-03 | url-status = dead }}</ref> While most supernovae are of the relatively homogeneous type II-P and are produced by red supergiants, blue supergiants are observed to produce supernovae with a wide range of luminosities, durations, and spectral types, sometimes sub-luminous like SN 1987A, sometimes super-luminous such as many type IIn supernovae.<ref name=mauerhan>{{cite arXiv|eprint=1209.6320v2|author1=Mauerhan|author2=Nathan Smith|author3=Alexei Filippenko|author4=Kyle Blanchard|author5=Peter Blanchard|author6=Casper|author7=Bradley Cenko|author8=Clubb|author9=Daniel Cohen|title=The Unprecedented Third Outburst of SN 2009ip: A Luminous Blue Variable Becomes a Supernova|class=astro-ph.SR|date=2012}}</ref><ref name=kleiser>{{cite journal | last1 = Kleiser | first1 = I. | last2 = Poznanski | first2 = D. | last3 = Kasen | first3 = D. | last4 = Filippenko | first4 = A. V. | last5 = Chornock | first5 = R. | last6 = Ganeshalingam | first6 = M. | last7 = Kirshner | first7 = R. P. | last8 = Li | first8 = W. | last9 = Matheson | first9 = T. | title = The Peculiar Type II Supernova 2000cb | date = 2011 | journal = Bulletin of the American Astronomical Society | volume = 43 | bibcode = 2011AAS...21733726K | page = 33726 |display-authors=3}}</ref><ref name=georgy>{{Cite journal | last1 = Georgy | first1 = C. | doi = 10.1051/0004-6361/201118372 | title = Yellow supergiants as supernova progenitors: An indication of strong mass loss for red supergiants? | journal = Astronomy & Astrophysics | volume = 538 | pages = L8–L2 | year = 2012 | pmid = | pmc = |arxiv = 1111.7003 |bibcode = 2012A&A...538L...8G }}</ref>