… Otherwise the jet stalls and deposits into the cocoon all its energy, E j = L j T, where T is
the engine operating time. The cocoon contains the stellar mass within a cone with a half …

Merging neutron stars offer an excellent laboratory for simultaneously studying strong-field
gravity and matter in extreme environments. We establish the physical association of an …

… To enhance the colour contrast, we change the normalization scale of ρ/ρ max and P/P
max in the third and fourth row in order to capture the tenuous material and pressure spilling …

… expression for t b in terms of the cocoon parameters a, b, and E 0 : … P c (t). If losses are
unimportant, the total cocoon energy, E 0 , can be treated as constant, so that P c (t) ∝ E 0 /V c (t). …

… Assuming that p eng is smooth and does not vary on short timescales in the vicinity of t B ,
then for T 90 ≪ t B , dN/dT 90 ≃ p eng (t B ), which is a constant, independent of T 90 . Indeed, …

… When using an electron energy power-law index p = 2.5 for the top-hat simulation, we find
the functional dependence on p is in a very good agreement with the one given in Nakar et al. …

… The thermal energy per baryon is given by w − m p c 2 , where w and m p are the enthalpy
per baryon and the proton mass, respectively. An extreme assumption for a baryonic outflow …

… ε e = 0.1, ε B = 0.01 (where ε e and ε B are the fraction of shock energy carried by the electrons
and by the magnetic field, respectively) and electron energy injection power-law index p = …

… Nakar and Piran 2002b have shown that in practically all long bursts the second-highest
peak is comparable in height to the first one. Thus if the highest peak is above the noise the sec…

… We fix the electron energy power-law index to p = 2.4 (we will comment on this point below
for each burst). We also fix the fraction of shocked energy in electrons to ϵ e = 0.2, since ϵ e …