@article{17639,
  abstract     = {It has been proposed that primordial gas in early dark matter halos, with virial temperatures above 10^4 K, can avoid fragmentation and undergo rapid collapse, possibly resulting in a supermassive black hole (SMBH). This requires the gas to avoid cooling and to remain at temperatures near T=10^4 K. We show that this condition can be satisfied in the presence of a sufficiently strong primordial magnetic field, which heats the collapsing gas via ambipolar diffusion. If the field has a strength above B = 3.6 (comoving) nG, the collapsing gas is kept warm (T=10^4K) until it reaches the critical density n_crit=10^3 cm^{-3} at which the roto-vibrational states of H_2 approach local thermodynamic equilibrium. H_2-cooling then remains inefficient, and the gas temperature stays near 10^4K, even as it continues to collapse to higher densities. The critical magnetic field strength required to permanently suppress H_2-cooling is somewhat higher than upper limit of approx. 2 nG from the cosmic microwave background (CMB). However, it can be realized in the rare (2-3)-sigma regions of the spatially fluctuating B-field; these regions contain a sufficient number of halos to account for the z=6 quasar BHs.},
  author       = {Sethi, Shiv and Haiman, Zoltán and Pandey, Kanhaiya},
  issn         = {0004-637X},
  journal      = {The Astrophysical Journal},
  number       = {1},
  pages        = {615--621},
  publisher    = {American Astronomical Society},
  title        = {{Supermassive black hole formation at high redshifts through a primordial magnetic field}},
  doi          = {10.1088/0004-637x/721/1/615},
  volume       = {721},
  year         = {2010},
}