The Direct Collapse of a Massive Black Hole Seed Under the Influence of an Anisotropic Lyman-Werner Source

Abstract

The direct collapse model of supermassive black hole seed formation provides an attractive solution to the origin of the quasars now routinely observed at $z\gtrsim 6$. We use the adaptive mesh refinement code Enzo to simulate the collapse of gas at high redshift, including a nine species chemical model of H, He, and H${}_2$. The direct collapse model requires that the gas cools predominantly via atomic hydrogen. To this end we simulate the effect of an anisotropic radiation source on the collapse of a halo at high redshift. The radiation source is placed at a distance of 3 kpc (physical) from the collapsing object. The source is set to emit monochromatically in the center of the Lyman-Werner (LW) band only at $12.8\mathrm{eV}$. The LW radiation emitted from the high redshift source is followed self-consistently using ray tracing techniques. We find that, due to self-shielding, a small amount of H${}_2$ is able to form at the very center of the collapsing halo even under very strong LW radiation. Furthermore, we find that a radiation source, emitting $>10^{54}(\sim 10^3{\mathrm{J}}_{21})$ photons per second is required to cause the collapse of a clump of $\mathrm{M}\sim 10^5$ M${}_{\odot }$. The resulting accretion rate onto the collapsing object is $\sim 0.25$ M${}_{\odot }$ $\mathrm{y}{\mathrm{r}}^{-1}$. Our results display significant differences, compared to the isotropic radiation field case, in terms of H${}_2$ fraction at an equivalent radius. These differences will significantly effect the dynamics of the collapse. With the inclusion of a strong anisotropic radiation source, the final mass of the collapsing object is found to be $\mathrm{M}\sim 10^5$ M${}_{\odot }$. This is consistent with predictions for the formation of a supermassive star or quasi-star leading to a supermassive black hole.

arXiv comment18 pages. ApJ accepted, with minor changes to submitted version. High resolution movies available at http://www.helsinki.fi/~regan/visualisations.html

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