A symbiotic scenario for the rapid formation of supermassive black holes

Abstract

Abstract. The most massive black holes, lurking at the centers of large galaxies, must have formed less than a billion years after the big bang, as they are visible today in the form of bright quasars at redshift larger than six. Their early appearance is mysterious, because the radiation pressure, generated by infalling ionized matter, inhibits the rapid growth of these black holes from stellar-mass black holes. It is shown that the supermassive black holes may form timeously through the accretion of predominantly degenerate sterile neutrino dark matter onto stellar-mass black holes. Our symbiotic scenario relies on the formation of, first, supermassive degenerate sterile neutrino balls through gravitational cooling and, then, stellar-mass black holes through supernova explosions of massive stars at the center of the neutrino balls. The observed lower and upper limits of the supermassive black holes are explained by the corresponding mass limits of the preformed neutrino balls.

Chern–Simons modified general relativity

“…In the context of CS gravity, the trajectory of sterile neutrinos would be controlled by the modified Dirac equation [6], which could now be studied in the new CS-modified, slow-rotating background of Yunes and Pretorius [84]. A modification in the behavior of fermions in highly-dense, strongly-gravitating systems could change the rate of black hole formation, such as in the the symbiotic supermassive formation mechanism [191].…”

“…5, the main effect of the CS correction on the propagation of GWs is an amplitude birefringence, characterized by the parameter ζ defined in Eq. (191). Thus, if a GW detection can constrain the magnitude of ζ, one can derive a bound on the CS scalar.…”

Neutrino masses, dark matter and the mysterious early quasars

“…This is based on a generalized LaneEmden equation, that describes the growth of a time-dependent point source, surrounded by a time-dependent degenerate sterile neutrino halo, such that the total mass is conserved and the steady-state flow obeys Bernoulli's equation [4]. Thus, in this partly nonrelativistic scenario, the most massive black holes may form between 650 and 840 Myr after the big bang.…”

“…at the center of M87, has at t = 13.7 Gyr and z ≈ 0 the same mass as the most massive quasar at t = 0.85 Gyr and z = 6.42. Thus the accretion of pre-concentrated dark matter onto stellar-mass black holes seems to be an attractive way to bypass the Eddington limit [4] that works against rapid spherical baryonic matter accretion.…”

Dark halo microphysics and massive black hole scaling relations in galaxies

“…In this case, a degenerate phase can act as a cored polytrope with F = 3 (e.g. Munyaneza & Biermann 2005, 2006Richter, Tupper & Viollier 2006;Chan & Chu 2008;Destri, de Vega & Sanchez 2013). For fermionic DM, the Pauli exclusion principle implies a universal maximum phase-space density, Q Qmax.…”