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Lepton asymmetry leading to baryogenesis by primordial black holes

Mriganka Dutta, Banibrata Mukhopadhyay, Abhishek Kumar Jha, Mayank Pathak, Siba Prasad Das

Abstract

Baryogenesis remains an unresolved problem in cosmology, with existing mechanisms facing significant caveats. We show that the effects of primordial black holes (PBHs) on neutrinos produce the lepton asymmetry $\sim 10^{-10}$ which subsequently produces the baryon asymmetry. We consider the Dirac Lagrangian in curved spacetime in local coordinates exhibiting Hermitian pseudo-vector and non-Hermitian vector terms. These terms lead to energy splitting between weakly interacting neutrinos and antineutrinos, resulting in their unequal number densities and hence a lepton asymmetry. While the non-Hermitian effect leads to a non-conserved total probability of neutrinos, the leptogenesis due to gravitational effects of a PBH could be significant until the nucleosynthesis era. This in turn produces baryon asymmetry from the symmetry of lepton and baryon numbers via the sphaleron process in the electro-weak era. We show that in the most conservative scenario, the PBHs of mass $\sim 10^{12}$ g and spin $\sim 0.01$ produce the observed baryogenesis at temperature 130 GeV, when such PBHs are available abundantly. However, massive PBHs also could produce the observed asymmetry, assuming the non/anti-Hermitian vector couplings for neutrino and anti-neutrino get canceled from the Lagrangian, leading the system to be Hermitian.

Lepton asymmetry leading to baryogenesis by primordial black holes

Abstract

Baryogenesis remains an unresolved problem in cosmology, with existing mechanisms facing significant caveats. We show that the effects of primordial black holes (PBHs) on neutrinos produce the lepton asymmetry which subsequently produces the baryon asymmetry. We consider the Dirac Lagrangian in curved spacetime in local coordinates exhibiting Hermitian pseudo-vector and non-Hermitian vector terms. These terms lead to energy splitting between weakly interacting neutrinos and antineutrinos, resulting in their unequal number densities and hence a lepton asymmetry. While the non-Hermitian effect leads to a non-conserved total probability of neutrinos, the leptogenesis due to gravitational effects of a PBH could be significant until the nucleosynthesis era. This in turn produces baryon asymmetry from the symmetry of lepton and baryon numbers via the sphaleron process in the electro-weak era. We show that in the most conservative scenario, the PBHs of mass g and spin produce the observed baryogenesis at temperature 130 GeV, when such PBHs are available abundantly. However, massive PBHs also could produce the observed asymmetry, assuming the non/anti-Hermitian vector couplings for neutrino and anti-neutrino get canceled from the Lagrangian, leading the system to be Hermitian.
Paper Structure (13 sections, 20 equations, 4 figures)

This paper contains 13 sections, 20 equations, 4 figures.

Table of Contents

  1. Introduction
  2. Number Densities for Neutrino and Anti-neutrino
  3. Energy dispersion relation
  4. Number density
  5. Neutrino--anti-neutrino transition probability
  6. Asymmetry around a black hole
  7. Potentials in Kerr metric
  8. Neutrino Asymmetry
  9. Primordial black hole
  10. Astrophysical black holes
  11. Viable parameter regime
  12. Asymmetry without violating Hermiticity
  13. Conclusion

Figures (4)

  • Figure 1: The variation of $A_0$ and $B^0$ as functions of (a)-(b) coordinate $\theta$ of BH spacetime at $r=2.1$, and (c) distance from BH for $\theta=\pi/4$, where BH mass $M=10^{-18}M_{\odot}$. In Fig. \ref{['1_fig:subb']}, $B^0$ for $a=0.01$ is multiplied by 500 to keep in the same scale as of $a=0.1$ in the plot.
  • Figure 2: Variation of neutrino asymmetry as a function of (a) BH mass for various spin, and (b) BH spin for various mass, at $r=2.1$ and $T=130~ \mathrm{GeV}$. The dot-dashed horizontal line indicates $10^{-10}$ level.
  • Figure 3: Three dimensional surface of $\Delta N=10^{-10}$ at $r=2.1$ in the ranges of BH mass, spin, and early universe temperature.
  • Figure 4: Variation of $\Delta N$ of the Hermitian case at $r=2.1$ as a function BH mass for various temperature of universe for a fixed spin $a=0.01$.