Abstract
The electromagnetic model assumes that rotational energy of a relativistic, stellar‐mass central source (black‐hole‐accretion disk system or fast rotating neutron star) is converted into magnetic energy through unipolar dynamo mechanism, propagated to large distances in a form of relativistic, subsonic, Poynting flux‐dominated wind and is dissipated directly into emitting particles through current‐driven instabilities. Collimating effects of magnetic hoop stresses lead to strongly non‐spherical expansion and formation of jets. Long and short GRBs may develop in a qualitatively similar way, except that in case of long burst ejecta expansion has a relatively short, non‐relativistic, strongly dissipative stage inside the star.
Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
