Matthew Bate's AnimationsCopyright and other information can be found at the bottom of this page.The dependence of stellar properties on metallicity (2019)![]() Reference: Bate 2019;
Date first added: 01/2019;
On the diversity and statistical properties of protostellar discs (2018)![]() Reference: Bate 2018;
Date first added: 01/2018;
On the dynamics of dust during protostellar collapse (2016)![]() Reference: Bate & Loren-Aguilar 2016;
Date first added: 11/2016;
Toridal vortices as a solution to the dust migration problem (2016)![]() Reference: Loren-Aguilar & Bate 2016;
Date first added: 01/2016;
Toridal vortices and the conglomeration of dust into rings in protoplanetary discs (2015)![]() Reference: Loren-Aguilar & Bate 2015;
Date first added: 07/2015;
The dependence of star cluster formation on metallicity (2014)![]() Reference: Bate 2014;
Date first added: 01/2014;
Stellar core and outflow formation in RMHD simulations (2014)![]() Reference: Bate, Tricco & Price 2014; Date first added: 10/2013; Star cluster formation in a 500 solar-mass cloud including radiative feedback (2012)![]() Reference: Bate 2012;
Date first added: 07/2011;
The formation and evolution of pre-stellar discs (2011)![]() Reference: Bate 2011; Date first added: 07/2011; Star cluster formation including radiative feedback (2009)![]() Reference: Bate 2009b;
Date first added: 10/2008;
The largest, most complex hydrodynamical star formation calculation ever performed (2009)![]() Reference: Bate 2009a Star cluster formation calculations (2002-2005)![]() 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. 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. 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.
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.![]() More 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). |