Gamma‐ray bursts: afterglows from cylindrical jets

Nearly all previous discussions on beaming effects in gamma‐ray bursts (GRBs) have assumed a conical geometry. However, more and more observations on relativistic jets in radio galaxies, active galactic nuclei, and ‘microquasars’ in the Galaxy have shown that many of these outflows are not conical, but cylindrical, i.e. they maintain constant cross‐sections at large scales. Thus it is necessary to discuss the possibility of gamma‐ray bursts being due to highly collimated cylindrical jets, not conical ones. Here we study the dynamical evolution of cylindrical jets and discuss their afterglows. Both analytical and numerical results are presented. It is shown that when the lateral expansion is not taken into account, a cylindrical jet typically remains highly relativistic for ∼ 10 8 –10 9  s . During this relativistic phase, the optical afterglow at first decays as S ∝ t −p/2 , where p is the index characterizing the power‐law energy distribution of electrons. Then the light curve steepens to S ∝ t −(p+1)/2 due to cooling of electrons. After entering the non‐relativistic phase (i.e. t≥10 11  s) , the afterglow is S ∝ t −(5p−4)/6 . However, if the cylindrical jet expands laterally at the comoving sound speed, then the decay becomes S ∝ t −p and S ∝ t −(15p−21)/10   –  t −(15p−20)/10 in the ultrarelativistic and in the non‐relativistic phase respectively. Note that in both cases the light curve turns flatter after the relativistic–Newtonian transition point, which differs markedly from the behaviour of a conical jet. It is suggested that some GRBs with afterglows decaying as t −1.1 –t −1.3 may be due to cylindrical jets, not necessarily isotropic fireballs.