Dynamical Stability of Six-dimensional Warped Flux Compactification (2005)
Yoshiguchi, Hiroyuki, Mukohyama, Shinji, Sendouda, Yuuiti, Kinoshita, Shunichiro
We show the dynamical stability of a six-dimensional braneworld solution with warped flux compactification recently found by the authors. We consider linear perturbations around this background...
Takami, Hajime, Yoshiguchi, Hiroyuki, Sato, Katsuhiko
We present numerical simulations on propagation of Ultra-High Energy Cosmic Rays (UHECRs) above $10^{19}$ eV in a structured extragalactic magnetic field (EGMF) and simulate their arrival...
Warped Flux Compactification and Brane Gravity (2005)
Mukohyama, Shinji, Sendouda, Yuuiti, Yoshiguchi, Hiroyuki, Kinoshita, Shunichiro
We find a simple exact solution of 6-dimensional braneworld which captures some essential features of warped flux compactification, including a warped geometry, compactification, a magnetic flux, and...
Quantization of scalar perturbations in brane-world inflation (2004)
Yoshiguchi, Hiroyuki, Koyama, Kazuya
We consider a quantization of scalar perturbations about a de Sitter brane in a 5-dimensional anti-de Sitter (AdS) bulk spacetime. We first derive the second order action for a master variable...
Yoshiguchi, Hiroyuki, Nagataki, Shigehiro, Sato, Katsuhiko
Recently, the High Resolution Fly's Eye (HiRes) experiment claims that there is no small scale anisotropy in the arrival distribution of ultra-high energy cosmic rays (UHECRs) above $E>10^{19}$ eV...
Bulk gravitational field and dark radiation on the brane in dilatonic brane world (2004)
Yoshiguchi, Hiroyuki, Koyama, Kazuya
We discuss the connection between the dark radiation on the brane and the bulk gravitational field in a dilatonic brane world model proposed by Koyama and Takahashi where the exact solutions for the...
Arrival Distribution of Ultra-High Energy Cosmic Rays: Prospects for the Future (2003)
Yoshiguchi, Hiroyuki, Nagataki, Shigehiro, Sato, Katsuhiko
We predict the arrival distribution of UHECRs above $4 \times 10^{19}$ eV with the event number expected by future experiments in the next few years. We perform event simulations with the source...