Matthew Bate's AnimationsCopyright and other information can be found at the bottom of this page.The dependence of star cluster formation on metallicity (2014)
Radiation hydrodynamical simulations of star formation in a 500 solar-mass molecular cloud with different metallicities, ranging from 1/100 to 3 times solar metallicity. More information.
Reference: Bate 2014;
Date first added: 01/2014;
Stellar core and outflow formation in RMHD simulations (2014)
Radiation magnetohydrodynamical simulations of the collapse of 1 solar-mass molecular cloud cores that follow the formation of the first core or pre-stellar disc, a slow magnetically-driven outflow from the first core, the second collapse and the formation of the stellar core, and the launching of a fast outflow from the vicinity of the stellar core. More information.
Reference: Bate, Tricco & Price 2014; Date first added: 10/2013; Star cluster formation in a 500 solar-mass cloud including radiative feedback (2012)
Radiation hydrodynamical simulations of star formation in a 500 solar-mass molecular cloud with high-quality animations. More information.
Reference: Bate 2012;
Date first added: 07/2011;
The formation and evolution of pre-stellar discs (2011)
Radiation hydrodynamical simulations of the collapse of 1 solar-mass molecular cloud cores that follow the formation of the first core or pre-stellar disc and its evolution before and after the formation of the stellar core within it. More information.
Reference: Bate 2011; Date first added: 07/2011; Star cluster formation including radiative feedback (2009)
Radiation hydrodynamical simulations of star formation in a 50 solar-mass molecular cloud with high-quality images and animations. More information.
Reference: Bate 2009b;
Date first added: 10/2008;
The largest, most complex hydrodynamical star formation calculation ever performed (2009)
Star formation in a 500 solar-mass molecular cloud with high-quality images and animations. More information.
Reference: Bate 2009a Star cluster formation calculations (2002-2005)
Quicktime, AVI and MPEG-4
32-747 MBytesThe 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. 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
AVI (13MB)
AVI (160MB)
Quicktime (22MB)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. Reference:
Bate, Bonnell & Price 1995 Date added: 06/2003
The evolution of a protobinary stellar system as it accretes from a gaseous envelope.
MPEG-1 1.4 MBInitial properties of the molecular cloud core: Uniform density, solid-body rotation. More information.
Reference: Bate 2000
Date added: 06/2001
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.
MPEG-1 2.0 MBMore information. Reference:
Bate 1998
Date added: 06/2001
About these pagesMany of the theoretical calculations I conduct during my research into star and planet formation result in animations. I will endevour to place as many of these computer simulations as I can on this page. New animations will be added at the top of the page with the dates that they were added. 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). |
