The stellar energy loss by the scattering γγ→νν compared to the plasmon decay
碩士 === 國立交通大學 === 物理研究所 === 88 === Energy loss is an important phenomenon for the explosion of supernovae and the creation of neutron stars. The plasmon decay γ→νν is known to be the dominant stellar energy-loss mechanism in the standard model. On the other hand, the scattering γγ→νν, ind...
| Main Authors: | , |
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| Format: | Others |
| Language: | en_US |
| Published: |
2000
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| Online Access: | http://ndltd.ncl.edu.tw/handle/61834840910038132246 |
| Summary: | 碩士 === 國立交通大學 === 物理研究所 === 88 === Energy loss is an important phenomenon for the explosion of supernovae and the creation of neutron stars. The plasmon decay γ→νν is known to be the dominant stellar energy-loss mechanism in the standard model. On the other hand, the scattering γγ→νν, induced by the scalar-scalar four-fermion interaction has a much larger cross section than its counterpart in the standard model.
In this document, we study the energy emission rate by the γγ→νν process in the model mentioned above, and compare this rate with that of the plasmon decay in the standard model.
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