Context :

Aims : We investigate the influence of ram-pressure stripping on the star formation and the mass distribution in simulated spiral galaxies .
Special emphasis is put on the question where the newly formed stars are located .
The stripping radius from the simulation is compared to analytical estimates .

Methods : Disc galaxies are modelled in combined N-body/hydrodynamic simulations ( GADGET-2 ) with prescriptions for cooling , star formation , stellar feedback , and galactic winds .
These model galaxies move through a constant density and temperature gas , which has parameters comparable to the intra-cluster medium ( ICM ) in the outskirts of a galaxy cluster ( T=3 keV \approx 3.6 \times 10 ^ { 7 } K and \rho =10 ^ { -28 } g/cm ^ { 3 } ) .
With this numerical setup we analyse the influence of ram-pressure stripping on the star formation rate of the model galaxy .

Results : We find that the star formation rate is significantly enhanced by the ram-pressure effect ( up to a factor of 3 ) .
Stars form in the compressed central region of the galaxy as well as in the stripped gas behind the galaxy .
Newly formed stars can be found up to hundred kpc behind the disc , forming structures with sizes of roughly 1 kpc in diameter and with masses of up to 10 ^ { 7 } M _ { \odot } .
As they do not possess a dark matter halo due to their formation history , we name them ’ stripped baryonic dwarf ’ galaxies .
We also find that the analytical estimate for the stripping radius from a Gunn & Gott ( 1972 ) criterion is in good agreement with the numerical value from the simulation .
Like in former investigations , edge-on systems lose less gas than face-on systems and the resulting spatial distribution of the gas and the newly formed stars is different .

Conclusions :