2012/10/28 by Prasanta Kumar Das, Das, Prasanta Kumar, J. Selvaganapathy +9
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #High Energy Physics - Phenomenology (hep-ph) #Neutrino Physics Research #astro-ph.HE #hep-ph
paper · pdf · doi:10.48550/arxiv.1210.7407
18 pages, 8 eps figures. arXiv admin note: substantial text overlap with arXiv:0801.1269; and with arXiv:hep-ph/0201099 by other authors
arxiv created 2012/10/28 · openalex publication_date 2012/10/28 · arxiv updated 2012/10/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In the Randall-Sundrum model where the Standard Model fields are confined to the TeV brane located at the orbifold point θ= π and the gravity peaks at the Planck brane located at θ= 0, the stabilized modulus (radion) field is required to stabilize the size of the fifth spatial dimension. It can be produced copiously inside the supernova core due to nucleon-nucleon bremstrahlung, electron-positron and plasmon-plasmon annihilations, which then subsequently decays to neutrino-antineutrino pair and take away the energy released in SN1987A explosion. Assuming that the supernovae cooling rate ε ≤ 7.288× 10-27 \rmGeV, we find the lower bound on the radion vev \vphi ∼ 9.0 TeV, 2.2 TeV and 0.9 TeV corresponding to the radion mass mϕ= 5 GeV, 20 GeV and 50 GeV, respectively.