  There is increasing evidence that low mass stars with circumstellar disks can
be born close to massive stars, in some cases within tenths of a pc. If the
disks have lifetimes greater than those of the more massive stars, they are
exposed to the radiation fields and gas flows from the late evolutionary phases
and supernovae of the massive stars. The fast flows from supernovae are likely
to give some stripping of mass from the disks, but do not typically lead to
complete disruption of the disks. In the slow wind from a red supergiant star,
there is the possibility of gravitational accretion of wind matter onto the
circumstellar disk. In the supernova explosion of a red supergiant, the
radiative flux at the time of shock breakout can heat and ionize a nearby disk,
leading to transient, narrow line emission. There are consequences for the
solar nebula if it was born ~0.2 pc from a massive star that became a red
supergiant. Accretion from the wind could supply a substantial amount of 26Al
to the disk. The high radiative luminosity of the eventual supernova could lead
to the melting of dust grains and the formation of chondrules. The passage of
the supernova ejecta could drive a shock wave in the disk, heating it.

Astrophysics