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We investigate how ram pressure of intragroup and intracluster medium caninfluence the spatial and temporal variations of star formation (SF) of diskgalaxies with halo masses (M_h) ranging from 10^10 M_sun to 10^12 M_sun (i.e.,from dwarf irregular to Milky Way-type) in groups and clusters with 10^13 <M_h/M_sun < 10^15 by using numerical simulations with a new model fortime-varying ram pressure. The long-term evolution of SF rates and H_alphamorphologies corresponding to the distributions of star-forming regions areparticularly investigated for different model parameters. The principal resultsare as follows. Whether ram pressure can enhance or reduce SF depends on M_h ofdisk galaxies and inclination angles of gas disks with respect to their orbitaldirections for a given orbit and a given environment. For example, SF can bemoderately enhanced in disk galaxies with M_h=10^12 M_sun at the pericenterpassages in a cluster with M_h=10^14 M_sun whereas it can be completely shutdown (`quenching') for low-mass disks with M_h=10^10 M_sun. Ram pressure canreduce the H_alpha-to-optical-disk-size ratios of disks and the revel of thereduction depends on M_h and orbits of disk galaxies for a given environment.Disk galaxies under strong ram pressure show characteristic H_alphamorphologies such as ring-like, one-sided, and crescent-like distributions.

Galactic star formation enhanced and quenched by ram pressure in groups and clusters