  We have calculated the two-point correlation functions in redshift space,
xi(sigma,pi), for galaxies of different spectral types in the 2dF Galaxy
Redshift Survey. Using these correlation functions we are able to estimate
values of the linear redshift-space distortion parameter, beta = Omega_m^0.6/b,
the pairwise velocity dispersion, a, and the real-space correlation function,
xi(r), for galaxies with both relatively low star-formation rates (for which
the present rate of star formation is less than 10% of its past averaged value)
and galaxies with higher current star-formation activity. At small separations,
the real-space clustering of passive galaxies is very much stronger than that
of the more actively star-forming galaxies; the correlation-function slopes are
respectively 1.93 and 1.50, and the relative bias between the two classes is a
declining function of radius. On scales larger than 10 h^-1 Mpc there is
evidence that the relative bias tends to a constant, b(passive)/b(active) ~ 1.
This result is consistent with the similar degrees of redshift-space
distortions seen in the correlation functions of the two classes -- the
contours of xi(sigma,pi) require beta(active)=0.49+/-0.13, and
beta(passive)=0.48+/-0.14. The pairwise velocity dispersion is highly
correlated with beta. However, despite this a significant difference is seen
between the two classes. Over the range 8-20 h^-1 Mpc, the pairwise velocity
dispersion has mean values 416+/-76 km/s and 612+/-92 km/s for the active and
passive galaxy samples respectively. This is consistent with the expectation
from morphological segregation, in which passively evolving galaxies
preferentially inhabit the cores of high-mass virialised regions.
