  In this review I discuss the various gamma-ray emission lines that are
expected and have been observed from radioactive explosive nucleosynthesis
products. The most important gamma-ray lines result from the decay chains of
Ni-56, Ni-57, and Ti-44. Ni-56 is the prime explosive nucleosynthesis product
of Type Ia supernovae, but Ni-56 is also a product of core-collapse supernovae.
Gamma-ray line emission from its daughter product, Co-56, has been detected
from SN1987A. The early occurrence of this emission indicates that some
fraction of Ni-56, which is synthesized in the innermost supernova layers, must
have mixed with the outermost ejecta.
  Special attention is given to the gamma-ray line emission of the decay chain
of Ti-44, giving line emission at 68 keV, 78 keV, and 1157keV. Given its decay
time of 86 yr, one expects this line emission from young supernova remnants.
The Ti-44 production is very sensitive to the explosion properties This makes
Ti-44 an ideal tool to study the inner layers of the supernova explosion.
  The gamma-ray line emission from Ti-44 has so far only been detected from the
supernova remnant Cas A. I discuss these detections, which were made by COMPTEL
and BeppoSAX, which suggest a Ti-44 yield of (1.5+/-1.0)x10^{-4} Msun.
Moreover, I present some preliminary results of Cas A observations by INTEGRAL,
which has yielded a 3sigma detection of the 68 keV line with the ISGRI
instrument at a level consistent with the BeppoSAX results. A preliminary
analysis of the vailable INTEGRAL-SPI data indicates that narrow line emission
(Delta v < 1000 km/s) can be almost excluded at the 2sigma level. (Abridged)
