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Simulation Movies

Simulation of a fragmenting disc

D. Stamatellos, A. Whitworth

Circumstellar disc fragmenting to produce a swarm of brown dwarfs. These are stars with such low masses that they never become hot enough to convert hydrogen into helium. They are very hard to detect because they have very low luminosities. gif [14.82 MB] mpg [14.02 MB]

Energeti radiaton from a newly-formed massive star ionizes and heats the surrounding gas

Detail of
          energeti radiaton.
T. Bisbas, A. Whitworth, & R. Wunsch

The neutral gas is accelerated to high speeds like a rocket. This is why the intersteallar medium is so turbulent. mpg [5.53 MB]

Clump in Molecular Cloud

Clump detail.
T. Bisbas, A. Whitworth, & R. Wunsch

A clump in a molecular cloud is overun by a shock-front driven by the radiation from a massive star, and collapses to form a small group of protostars. mpg [1.76 MB]

Self-propagating star formation

R. Wunsch & A. Whitworth

The wind from a massive star has swept up a dense shell of mater which breaks up to form a new generation of protostars. This process can repeat itself to produce an epidemic of star formation. mpg [1.20 MB]

The formation of super star clusters

R. Wunsch

Super star clusters formed in colliding galaxies drive powerful winds which deposit heavy elements in the intergalactic medium. At the same time, a second generation of stars can be formed from the cooling wind material in the centre of the galaxy. mpg [1.62 MB]

Star formation in turbulent clouds

Attwood, Stamatellos, Whitworth

A dense molecular cloud collapses to form a small cluster of stars. Stars form with a wide range of masses (from less than 0.01 Msun to more than 100 Msun). Most stars are born in binary systems. mpg [10.76 MB]

Star formation in spiral galaxies

McLeod, Whitworth

The patterns of star formation in a spiral galaxy like our own Milky way, which has been disturbed by a passing by galaxy. mpg [10 MB]