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The increasing observed number of supernova events allows for finding evermore frequently the progenitor star in archive images. In a few cases, theprogenitor star is a yellow supergiant star. The estimated position in theHertzsprung-Russell diagram of these stars is not compatible with thetheoretical tracks of classical single star models. According to severalauthors, the mass-loss rates during the red supergiant phase could beunderestimated. We study the impact of an increase of these mass-loss rates onthe position of 12 to 15 M\odot stars at the end of their nuclear life, inorder to reconcile the theoretical tracks with the observed yellow supergiantprogenitors. We perform calculations of 12 to 15 M\odot rotating stellar modelsusing the Geneva stellar evolution code. To account for the uncertainties inthe mass-loss rates during the RSG phase, we increase the mass-loss rate of thestar (between 3 and 10 times the standard one) during that phase and comparethe evolution of stars undergoing such high mass-loss rates with modelscomputed with the standard mass-loss prescription. We show that the finalposition of the models in the Hertzsprung-Russell diagram depends on the massloss they undergo during the red supergiant phase. With an increased mass-lossrate, we find that some models end their nuclear life at positions that arecompatible with the observed position of several supernova progenitors. Weconclude that an increased mass-loss rate (whom physical mechanism still needto be clarified) allows single star models to reproduce simultaneously theestimated position in the HRD of the YSG SN progenitors, as well as the SNtype.

Yellow supergiants as supernova progenitors: an indication of strong mass loss for red supergiants?