Abstract
We revise existing limits on the D-dimensional Planck scale M_D from the nonobservation of microscopic black holes produced by high energy cosmic neutrinos in scenarios with D=4+n large extra dimensions. Previous studies have neglected the energy radiated in gravitational waves by the multipole moments of the incoming shock waves. We include the effects of energy loss, as well as form factors for black hole production and recent null results from cosmic ray detectors. For n>4, we obtain M_D > 1.0 - 1.4 TeV. These bounds are among the most stringent and conservative to date.
Highlights
Forthcoming colliders1͔, cosmic ray observatories2– 4͔, neutrino telescopes5͔, and space-based experiments6͔ will be able to observe black holesBHsif the fundamental scale of gravity is sufficiently close to 1 TeV7͔
We revise existing limits on the D-dimensional Planck scale M D from the nonobservation of microscopic black holes produced by high energy cosmic neutrinos in scenarios with Dϭ4ϩn large extra dimensions
We include the effects of energy loss, as well as form factors for black hole production and recent null results from cosmic ray detectors
Summary
Forthcoming colliders1͔, cosmic ray observatories2– 4͔, neutrino telescopes5͔, and space-based experiments6͔ will be able to observe black holesBHsif the fundamental scale of gravity is sufficiently close to 1 TeV7͔. Analytic calculations in four dimensions10,11͔ for head-on collisions illustrated the process of horizon formation and found that the mass of the final BH was about 84% of the initial center-of-mass energy These calculations were extended to nonzero impact parameter by Eardley and Giddings12͔, who analytically derived a lower bound on the total cross section of approximately 65% of Eq ͑1͒. Recently, a calculation of the cross section in higher dimensions was performed by Yoshino and Nambu using numerical techniques13͔ These authors observed significant reductions in the mass of the final-state black hole as a function both of impact parameter and dimension. Besides incorporating the cross section and energy loss results of Yoshino and Nambu, we make use of updated parton distribution functions and recently available cosmic ray data
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
