Utilizing a large sample of infrared-selected starburst galaxies havin
g optical images and long-slit spectra, we explore the interrelationsh
ips between the properties of starbursts and relate these properties t
o those of the ''host'' galaxy. We find that the half-light radius of
the Ha-emitting region (r(e,H alpha)) enters into several correlations
that suggest it is physically related to the actual starburst radius.
Most suggestively, the effective IR surface brightness (L(IR)/pi r(e,
H alpha)(2)) correlates strongly with the far-IR color temperature. Th
is can be reproduced roughly with an idealized model of a surrounding
dust screen whose far-IR emissivity is determined by the local energy
density of UV starburst light. Typical values for r(e,H alpha) are a f
ew hundred pc to a few kpc (with the Ha emission being significantly m
ore compact than the red starlight). This confirms the ''circumnuclear
'' scales of typical starbursts. We show also that starbursts seem to
obey a limiting IR surface brightness of about 10(11) L. kpc(2), corre
sponding to a maximum star formation rate of about 20 M. yr(-1) kpc(2)
for a normal initial mass function. We argue that this upper limit su
ggests that starbursts are self-regulating in some way. We show that m
ost of these galaxies have relatively normal, symmetric rotation curve
s. This implies that the galactic disk need not suffer severe dynamica
l damage in order to ''fuel'' a typical starburst. We show also that t
he starbursts occur preferentially in the inner region of solid-body r
otation. This may reflect both bar-driven inflow of gas to the region
between the inner Lindblad resonances and the dominance of gravitation
al instability over tidal shear in this region. Most of the starbursts
reside in galaxies with rotation speeds of 120-200 km s(-1) (compared
to 220 km s(-1) for a fiducial L galaxy like the Milky Way). The lac
k of a correlation between galaxy rotation speed and starburst luminos
ity means that even relatively modest galaxies (masses approximate to
10% of the Milky Way) can host powerful starbursts. We argue on the ba
sis of causality that the internal velocity dispersion in a starburst
sets an upper limit to the star formation rate. The most extreme starb
ursts approach this limit, but most are well below. Finally, we show t
hat the relative narrowness of the nuclear emission lines in starburst
s (relative to the galaxy rotation speed) arises because the gas in th
e nuclear ''bin'' usually does not sample fully the solid-body part of
the rotation curve. The narrow lines do not necessarily imply that th
e starburst is not in dynamical equilibrium.