5.1. Models for The Energy Flow
The simplest mode of relativistic energy flow is in the form of kinetic energy of relativistic particles. A variant that have been suggested is based on the possibility that a fraction of the energy is carried by Poynting flux [224, 225, 226, 69, 227] although in all models the power must be converted to kinetic energy somewhere. The energy flow of ~ 1050 ergs/sec from a compact object whose size is 107cm requires a magnetic field of 1015Gauss or higher at the source. This large value might be reached in stellar collapses of highly magnetized stars or amplified from smaller fields magnethohydrodynamically . Overall the different models can be characterized by two parameters: the ratio of the kinetic energy flux to the Poynting flux and the location of the energy conversion stage ( 1012 cm for internal conversion or 1016 cm for external conversion). This is summarized in Table 5.1. In the following section we will focus on the simplest possibility, that is of a kinetic energy flux.
|Kinetic Energy||Kinetic Energy and||Poynting Flux|
|Internal||[28, 29, 18]||||[225, 69, 227]|
|External||[27, 219]||-||[226, 69]|