  In the first paper of this series we used HI observations of the 19 brightest
spirals in Coma to analyze the dynamical state of the cluster. In this paper we
present the detailed HI distribution and kinematics of the spirals that were
detected in HI, and radio continuum data for a sample of star forming and post
starburst galaxies in Coma. We discuss the importance of ICM-ISM interactions
to explain the observed HI morphology. A rough comparison of observed HI sizes
with predicted HI sizes from simulations by Abadi et al. (1999) gives
reasonable agreement. We use the results on radio continuum emission to
estimate the star formation rate in the PSB galaxies we pointed at. The radio
continuum emission in the 11 so called post starburst galaxies, identified by
Caldwell et al. (1993) in the cluster, is weak. Eight of the 11 were not
detected down to a 3 sigma upper limit of 0.6 mJy. This sets an upper limit to
the star formation rate in these galaxies of less than 0.2 solar masses per
year. The three detected post starburst galaxies have a star formation rate of
less than one solar mass per year. Thus none of the post starburst galaxies in
Coma are dust enshrouded starbursts.
