The radio emission from supernovae
provides a direct probe of a supernova’s
circumstellar environment, which presumably was
established by mass-loss episodes in the late
stages of the progenitor’s presupernova evolution.
The observed synchrotron emission is generated by
the SN shock interacting with the relatively
high-density circumstellar medium which has been
fully ionized and heated by the initial UV/X-ray
flash. The study of radio supernovae therefore
provides many clues to and constraints on stellar
evolution. We will present the recent results on
several cases, including SN 1980K, whose recent
abrupt decline provides us with a stringent
constraint on the progenitor’s initial mass; SN
1993J, for which the profile of the wind matter
supports the picture of the progenitor’s evolution
in an interacting binary system; and SN 1979C,
where a clear change in presupernova mass-loss
rate occurred about 104 years
before explosion. Other examples, such as SNe
19941 and 1996cb, will also be discussed.