Theory Group


Cosmic Reionization

Early Universe

First Stars & Galaxies

Fundamental Physics

Structure Formation

Extragalactic Astrophysics

Clusters of Galaxies

Theoretical & Computational Astrophysics

Galactic Evolution

ISM and Star Formation

Milky Way Evolution

Planetary Sciences


Planet Formation

Stellar Astrophysics


Gamma-ray Bursts

Neutron Stars & Magnetars


White Dwarfs

Theory Group : Extragalactic Astrophysics : Theoretical & Computational Astrophysics

Early Universe Computational Astrophysics Laboratory

Volker Bromm, Milos Milosavljevic, Jeremy Ritter, Aaron Smith

ADS | astro-ph

Volker Bromm  



Research Interests

Formation of the first stars and quasars; high-redshift supernovae and metal enrichment; supermassive black hole formation; gamma-ray bursts; reionization of the intergalactic medium; present-day star formation; computational astrophysics.

Group Areas

Theory, First Stars & Galaxies, Structure Formation, Theoretical & Computational Astrophysics, ISM and Star Formation

ADS | astro-ph

Milos Milosavljevic  

Associate Professor


Research Interests

Massive black holes; the Galactic center; galaxy formation; galaxy clusters; plasma astrophysics.

Group Areas

Theory, Gamma-ray Bursts, Clusters of Galaxies, Theoretical & Computational Astrophysics, Black Holes & AGN

ADS | astro-ph

Jeremy Ritter  

Graduate Student

Research Interests

Computational Cosmology

Group Areas

Theory, First Stars & Galaxies, Theoretical & Computational Astrophysics

ADS | astro-ph

Aaron Smith  

Graduate Student


Research Interests

Lyman-α radiative transfer; the cosmic microwave background.

Group Areas

Theory, Early Universe, First Stars & Galaxies, Structure Formation, Theoretical & Computational Astrophysics

Gas number density n (upper panels) and neutral fraction XH (lower panels) at two separate instances around t~4,000 yr. The left panels show the flow during a central accretion minimum; infalling gas is clearly visible at r~1.5 x 1016 cm. The right panels show the flow during a central accretion maximum. The structure near the central axis, in the conical region marked by dashed lines, is an artifact of our having set the optical depth to zero along the axis, for R/|z| < tan5°, to avoid numerical issues arising from the coordinate singularity.


Accretion onto Intermediate-Mass Black Holes in Dense Protogalactic Clouds astro-ph