A possible mechanism for production of primordial black holes in early universe

Abstract

Primordial Black Hole Remnants(PBHRs) can be considered as a primary source of cold dark matter. Hybrid inflation provides a possible framework for production of primordial black holes(PBHs) and these PBHs evaporate subsequently to produce PBHRs. In this paper we provide another framework for production of these PBHs. Using signature changing cosmological model and the generalized uncertainty principle as our primary inputs, first we find a geometric cosmological constant for early stage of universe evolution. This geometric cosmological constant can lead to heavy vacuum density which may be interpreted as a source of PBHs production during the inflationary phase. In the next step, since it is possible in general to have non-vanishing energy-momentum tensor for signature changing hypersurface, this non-vanishing energy-momentum tensor can be considered as a source of PBHs production. These PBHs then evaporate via the Hawking process to produce PBHRs. Finally, possible observational schemes for detecting relics of these PBHRs are discussed. PACS Numbers: 98.80. Qc, 95.35.+d

Effect of Primordial Black Holes on the Cosmic Microwave Background and Cosmological Parameter Estimates

“…One interesting feature of this model is a huge bump in the power spectrum at kpc scales with overdensity δ > 1. Other possible scenarios for PBH formation involve non-Gaussian perturbations produced by cosmic strings, cosmic string collapse or bubble collisions following second-order phase transitions (e.g., Polnarev & Zembowicz 1991;Rubin et al 2001;Stojkovic et al 2005;Nozari 2007). It is generally considered unlikely that PBH formation occurred after t = 1 s, when M pbh ∼ M H > ∼ 10 5 M ⊙ , because the physics in this domain is sufficiently understood and their formation would affect primordial nucleosynthesis.…”

New cosmological constraints on primordial black holes

“…decrease with increasing scale) and this means that the PBHs form shortly after reheating [7][8][9][10]. Others involve some form of "designer" inflation, in which the power spectrum of the fluctuations-and hence PBH production-peaks on some scale [11][12][13][14][15][16][17][18][19][20][21][22][23][24][25]. In other scenarios, the fluctuations have a "running index," so that the amplitude increases on smaller scales but not according to a simple power law [26][27][28][29][30][31][32][33].…”

Primordial black holes

“…Various aspects of PBH physics, mechanisms of their formation, evolution and effects are discussed in Carr et al (1994); Carr & MacGibbon (1998); Liddle & Green (1998);MacGibbon et al (1998); Wichoski et al (1998); Chechetkin et al (1982a); Polnarev & Khlopov (1985); Grillo & Srivastava (1981); Chapline (1975); Hayward & Pavón (1989); Yokoyama (1997); Kim & Lee (1996); Heckler (1997);MacGibbon et al (2008); Page et al (2008); Green & Liddle (1997); Niemeyer & Jedamzik (1998); Kribs et al (1999); Green et al (2004); Yokoyama (1998aYokoyama ( ,b, 1999; Bringmann et al (2002); Dimopoulos & Axenides (2005); Nozari (2007); Lyth et al (2006); Zaballa et al (2007); Harada & Carr (2005a); Custódio & Horvath (2005); Bousso & Hawking (1995; Elizalde et al (1999); Nojiri et al (1999); Bousso & Hawking (1999); Silk (2000); Polarski (2002); Barrow & Carr (1996); Paul (2000); Paul et al (2002); Paul & Paul (2005); Polarski & Dolgov (2001);…”