Contact details:
I’m a PhD student at the Centre for Astrophysics and Supercomputing at Swinburne University in Melbourne, Australia and at the European Southern Observatory (ESO) in Santiago, Chile. My supervisor is Jarrod Hurley.
Currently I am carrying out my research in Chile.

research aims to better understand the evolution of star clusters of all sizes, and in particular I’m interested in the many things that have an influence on their evolution. That includes both, effects on large and small scales such as the influence of an external tidal field as well as the impact of stellar remnant black holes in the core of a cluster and in addition to that, effects originating from intrinsic properties, such as the chemical composition (metallicity) of the stars which make up the cluster.
To do so, I utilise the direct
N-body code NBODY6.


Multiple stellar-mass black holes in globular clusters: theoretical confirmation
Anna Sippel & Jarrod Hurley, MNRAS, 2012

Link to ADS and arXiv.

Screen Shot 2013-02-04 at 3.30.14 PM

N-body models of globular clusters: metallicities, half-light radii and mass-to-light ratios
Anna Sippel, Jarrod Hurley, Juan Madrid and William Harris, MNRAS, 2012

Link to
ADS and arXiv.

The Size Scale of Star Clusters
Juan Madrid, Jarrod Hurley and Anna Sippel, ApJ, 2012

Link to
ADS and arXiv.

Below is a
model of a young star cluster in real (albeit exaggerated) colours. The white box is not related to the simulation itself, but for illustrational purposes: it’s size is twice the distance from the sun to Alpha Centauri, the closest star visible to the naked eye. You can also see this image on the latest newsletter of the Australian National Institute for Theoretical Astrophysics (see here).

Below one can see the orbit of a newly formed stellar remnant black hole. In the very centre of this picture is a black hole with ten solar masses (red +). It has not received a large kick at formation and due to mass segregation settled down in the centre pretty quickly. The yellow + is showing a black hole with just five solar masses. At formation, it received a kick nearly ejecting it from the cluster. Marked in green + is the trail.


Since 2012, I am running these simulations on gSTAR, the new GPU supercomputer at Swinburne. There are hundreds of CPUs and more than 100 GPUs in the 11 cabinets you can see behind me. Evolving N-body models is computationally expensive, hence a good computer is very helpful!