2002/10/31 by Rong-Gen Cai, Yun Soo Myung · 24 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Einstein #Einstein equations #Entropy (arrow of time) #Gravitation #Holographic principle #Holography #Noncommutative and Quantum Gravity Theories #Upper and lower bounds #f(R) gravity #hep-th
paper · pdf · open access · doi:10.1016/s0370-2693(03)00303-4
published in Physics Letters B 559(1-2), 60-64 (Elsevier BV) · 8 pages, Latex
arxiv created 2002/10/31 · openalex publication_date 2003/04/01 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We discuss the holography and entropy bounds in Gauss–Bonnet gravity theory. By applying a Geroch process to an arbitrary spherically symmetric black hole, we show that the Bekenstein entropy bound always keeps its form as S B =2 πER , independent of gravity theories. As a result, the Bekenstein–Verlinde bound also remains unchanged. Along the Verlinde's approach, we obtain the Bekenstein–Hawking bound and Hubble bound, which are different from those in Einstein gravity. Furthermore, we note that when HR =1, the three cosmological entropy bounds become identical as in the case of Einstein gravity. But the corresponding Friedmann equation in Gauss–Bonnet gravity can no longer be cast to the form of cosmological Cardy formula.