  The increasing observed number of supernova events allows for finding ever
more frequently the progenitor star in archive images. In a few cases, the
progenitor star is a yellow supergiant star. The estimated position in the
Hertzsprung-Russell diagram of these stars is not compatible with the
theoretical tracks of classical single star models. According to several
authors, the mass-loss rates during the red supergiant phase could be
underestimated. We study the impact of an increase of these mass-loss rates on
the position of 12 to 15 M\odot stars at the end of their nuclear life, in
order to reconcile the theoretical tracks with the observed yellow supergiant
progenitors. We perform calculations of 12 to 15 M\odot rotating stellar models
using the Geneva stellar evolution code. To account for the uncertainties in
the mass-loss rates during the RSG phase, we increase the mass-loss rate of the
star (between 3 and 10 times the standard one) during that phase and compare
the evolution of stars undergoing such high mass-loss rates with models
computed with the standard mass-loss prescription. We show that the final
position of the models in the Hertzsprung-Russell diagram depends on the mass
loss they undergo during the red supergiant phase. With an increased mass-loss
rate, we find that some models end their nuclear life at positions that are
compatible with the observed position of several supernova progenitors. We
conclude that an increased mass-loss rate (whom physical mechanism still need
to be clarified) allows single star models to reproduce simultaneously the
estimated position in the HRD of the YSG SN progenitors, as well as the SN
type.
