Copyright: Unless otherwise stated, all of the material on this site is the property of Matthew Bate. Any of my pictures and animations may be used freely for non-profit purposes (such as during scientific talks) as long as appropriate credit is given wherever they appear. Permission must be obtained from me before using them for any other purpose (e.g. pictures for publication in books).

	Some of the largest and most complex star formation calculations ever performed. The first was press-released on April 12, 2002 with high-quality images and animations. Since then four large-scale calculations have been performed. More information.	FORMAT	SIZE
		Quicktime AVI MPEG-4	32-747 MBytes
	References: Bate, Bonnell, Bromm 2002a; Bate, Bonnell, Bromm 2002b; Bate, Bonnell, Bromm 2003 ; Bate & Bonnell 2005
	Date first added: 04/2002; Updated 09/2004
	Collapse and fragmentation of a molecular cloud core to form a triple system. A binary system forms first from an initial m=2 density perturbation in the cloud. Subsequently, one of the protostellar discs fragments to give a third object. The result is a stable triple system surrounded by a circumtriple disc.	FORMAT	SIZE
		AVI AVI Quicktime	13MB 160MB 22MB
	Reference: Bate, Bonnell & Price 1995
	Date added: 06/2003
	The evolution of a protobinary stellar system as it accretes from a gaseous envelope. Initial properties of the molecular cloud core: Uniform density, solid-body rotation. More information.	FORMAT	SIZE
		MPEG-1	1.4 MB
	Reference: Bate 2000
	Date added: 06/2001
	The evolution of a protobinary stellar system as it accretes from a gaseous envelope. Initial properties of the molecular cloud core: 1/r-density, solid-body rotation. More information.	FORMAT	SIZE
		MPEG-1	2.6 MB
	Reference: Bate 2000
	Date added: 06/2001
	The dynamical rotational instability of the first hydrostatic core that can occur during the collapse of a molecular cloud to form a star. More information.	FORMAT	SIZE
		MPEG-1	2.0 MB
	Reference: Bate 1998
	Date added: 06/2001