Many observed massive star-forming z \approx 2 galaxies are large disks that exhibit irregular morphologies , with \approx 1 { \thinspace kpc } , \approx 10 ^ { 8 - 10 } \hbox { $ \thinspace M _ { \odot } $ } clumps .
We present the largest sample to date of high-resolution cosmological SPH simulations that zoom-in on the formation of individual M _ { * } \approx 10 ^ { 10.5 } \hbox { $ \thinspace M _ { \odot } $ } galaxies in \approx 10 ^ { 12 } \hbox { $ \thinspace M _ { \odot } $ } halos at z \approx 2 .
Our code includes strong stellar feedback parameterized as momentum-driven galactic winds .
This model reproduces many characteristic features of this observed class of galaxies , such as their clumpy morphologies , smooth and monotonic velocity gradients , high gas fractions ( f _ { g } \approx 50 \% ) and high specific star-formation rates ( \gtrsim 1 { \thinspace Gyr } ^ { -1 } ) .
In accord with recent models , giant clumps ( M _ { clump } \approx ( 5 \times 10 ^ { 8 } -10 ^ { 9 } ) \hbox { $ \thinspace M _ { \odot } $ } ) form in-situ via gravitational instabilities .
However , the galactic winds are critical for their subsequent evolution .
The giant clumps we obtain are short-lived and are disrupted by wind-driven mass loss .
They do not virialise or migrate to the galaxy centers as suggested in recent work neglecting strong winds .
By phenomenologically implementing the winds that are observed from high-redshift galaxies and in particular from individual clumps , our simulations reproduce well new observational constraints on clump kinematics and clump ages .
In particular , the observation that older clumps appear closer to their galaxy centers is reproduced in our simulations , as a result of inside-out formation of the disks rather than inward clump migration .