Energy Loss of Neutrinos in and Massive Stars
- Conference date: 27–30 October 2010
- Location: Damai Laut, (Malaysia)
The progress from the theoretical and experimental aspects in neutrino physics shines light into neutrino physics as well as in astrophysics. It is known that when neutrinos pass through a medium, the neutrinos interact with electrons before emerging from the stars with an effective potential energy produced due to coherent forward scatterings that occurred in the medium. This potential engenders significant changes in the neutrino masses and their mixing in the medium. Thus electron neutrinos would oscillate into different mass eigenstate and this is dependent on the energy of the neutrinos. Some of the energy will be lost in the coherent scattering with the electrons by the charged current interaction. We have calculated the energy loss of the neutrinos by using a stopping power equation for both rotating and non‐rotating and stars. The total energy loss of neutrinos depends on the electron density in the stars and on the survival probability of the electron neutrino. For high electron density profile and the survival probability, the energy loss will be significant.
- Collisional energy loss
- Electron neutrinos
- Electron energy loss spectroscopy
- Electron scattering
- Forward scattering
- Neutrino interactions
- Neutrino mass
- Neutrino mixing
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Y. K. Semertzidis, M. Aoki, M. Auzinsh, V. Balakin, A. Bazhan, G. W. Bennett, R. M. Carey, P. Cushman, P. T. Debevec, A. Dudnikov, F. J. M. Farley, D. W. Hertzog, M. Iwasaki, K. Jungmann, D. Kawall, B. Khazin, I. B. Khriplovich, B. Kirk, Y. Kuno, D. M. Lazarus, L. B. Leipuner, V. Logashenko, K. R. Lynch, W. J. Marciano, R. McNabb, W. Meng, J. P. Miller, W. M. Morse, C. J. G. Onderwater, Y. F. Orlov, C. S. Ozben, R. Prigl, S. Rescia, B. L. Roberts, N. Shafer‐Ray, A. Silenko, E. J. Stephenson, K. Yoshimura and EDM Collaboration
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