2021/11/30 by Soma Heydari, Kayoomars Karami, K. Karami · 38 citations
Physics and Astronomy · #Amplitude #Astrophysics #Binary black hole #Cosmology and Gravitation Theories #Coupling (piping) #Coupling parameter #Exponential function #Galaxy #Gamma-ray bursts and supernovae #Gravitational microlensing #Gravitational wave #Inflation (cosmology) #Inflaton #LIGO #Light curve #Mathematical analysis #Mathematical physics #Physics #Primordial black hole #Pulsars and Gravitational Waves Research #Quantum mechanics #Reionization #Stars #astro-ph.CO #gr-qc #hep-th
paper · pdf · doi:10.1088/1475-7516/2022/03/033
published in Journal of Cosmology and Astroparticle Physics 2022(03), 033 (Institute of Physics) · 29 pages, 5 figures
openalex created_date 2021/11/08 · openalex publication_date 2022/03/01 · arxiv created 2022/03/16 · arxiv updated 2022/03/17 · openalex updated_date 2026/08/05
Here, Primordial Black Holes (PBHs) creation from exponential potential has been inquired, through gravitationally raised friction emanated from the nonminimal coupling between gravity and field derivative setup. Setting a two-parted exponential function of inflaton field as coupling parameter, and fine-tuning of four parameter cases of our model, we could sufficiently slow down the inflaton owing to high friction during an ultra slow-roll phase. This empowers us to achieve enough enhancement in the amplitude of curvature perturbations power spectra, via numerical solving of Mukhanov-Sasaki equation. Thereafter, we illustrate the generation of four PBHs with disparate masses in RD era, corresponding to our four parameter cases. Two specimens of these PBHs with stellar \cal O(10)M\odot and earth \cal O(10-6)M\odot masses can be appropriate to explicate the LIGO-VIRGO events, and the ultrashort-timescale microlensing events in OGLE data, respectively. Another two cases of PBHs have asteroid masses around \cal O(10-13)M\odot and \cal O(10-15)M\odot with abundance of 96% and 95% of the Dark Matter (DM) content of the universe. Furthermore, we scrutinize the induced Gravitational Waves (GWs) ensued from PBHs production in our model. Subsequently, we elucidate that their contemporary density parameter spectra (Ω\rm GW0) for all predicted cases have acmes which lie in the sensitivity scopes of the GWs detectors, thereupon the verity of our conclusions can be verified in view of deduced data from these detectors. At length, our numerical outcomes exhibit a power-law behavior for the spectra of Ω\rm GW0 with respect to frequency as Ω\rm GW0 (f) ∼ (f/fc)n in the proximity of acmes position. As well, in the infrared regime f≪ fc, the log-reliant form of power index as n=3-2/ln(fc/f) is attained.