  Solar jets are fast-moving, elongated brightenings related to ejections seen
in both images and spectra on all scales from barely visible chromospheric jets
to coronal jets extending up to a few solar radii. The largest, most powerful
jets are the source of type III radio bursts, energetic electrons and ions with
greatly enhanced $^3$He and heavy element abundances. The frequent coronal jets
from polar and equatorial coronal holes may contribute to the solar wind. The
primary acceleration mechanism for all jets is believed to be release of
magnetic stress via reconnection; however the energy buildup depends on the
jets' source environment. In this review, we discuss how certain features of
X-ray and EUV jets, such as their repetition rate and association with radio
emission, depends on their underlying photospheric field configurations (active
regions, polar and equatorial coronal holes, and quiet Sun).
