This paper presents a model for cosmological gamma-ray bursts (GRBs) based on unsteady outflows from compact stellar-mass objects. The key idea is that the energy released in a GRB is not released as a steady outflow but rather as an irregular one, allowing for internal shocks that can dissipate a significant fraction of the kinetic energy. This mechanism requires less extreme assumptions than previous models, such as lower values of the Lorentz factor Γ and less baryonic contamination. The paper discusses the dynamics of an unsteady relativistic outflow, where the mean Lorentz factor Γ is determined by the ratio of radiation and magnetic energy to rest mass (η). Variations in η over time can lead to internal shocks, which can convert kinetic energy into non-thermal radiation. The efficiency of this process depends on the relative velocities of the outflowing material and the timescale of the variations (t_var). The role of magnetic fields is also discussed. Strong magnetic fields can dominate the dynamics of the outflow, influencing the cooling processes and the formation of shocks. The magnetic field strength at the dissipation radius is found to be significant, and the synchrotron cooling time is shown to be short enough to ensure efficient radiative efficiency. The paper also addresses the phenomenology of GRBs, noting that the complex time structure of observed bursts may be due to irregularities in the outflow. The model suggests that the observed bursts could be due to either stellar collapse or compact binary mergers. The implications of this model are that the short timescales and adequate efficiencies do not require such high values of η as previously thought, and that the time structure of GRBs could be complex, depending on the history of the Lorentz factor. The model also suggests that the observed gamma rays are concentrated into an angle of order 1/η, implying a beamed or jet-like geometry. The energy sources in a cosmological context could be either stellar collapse or compact binary mergers.This paper presents a model for cosmological gamma-ray bursts (GRBs) based on unsteady outflows from compact stellar-mass objects. The key idea is that the energy released in a GRB is not released as a steady outflow but rather as an irregular one, allowing for internal shocks that can dissipate a significant fraction of the kinetic energy. This mechanism requires less extreme assumptions than previous models, such as lower values of the Lorentz factor Γ and less baryonic contamination. The paper discusses the dynamics of an unsteady relativistic outflow, where the mean Lorentz factor Γ is determined by the ratio of radiation and magnetic energy to rest mass (η). Variations in η over time can lead to internal shocks, which can convert kinetic energy into non-thermal radiation. The efficiency of this process depends on the relative velocities of the outflowing material and the timescale of the variations (t_var). The role of magnetic fields is also discussed. Strong magnetic fields can dominate the dynamics of the outflow, influencing the cooling processes and the formation of shocks. The magnetic field strength at the dissipation radius is found to be significant, and the synchrotron cooling time is shown to be short enough to ensure efficient radiative efficiency. The paper also addresses the phenomenology of GRBs, noting that the complex time structure of observed bursts may be due to irregularities in the outflow. The model suggests that the observed bursts could be due to either stellar collapse or compact binary mergers. The implications of this model are that the short timescales and adequate efficiencies do not require such high values of η as previously thought, and that the time structure of GRBs could be complex, depending on the history of the Lorentz factor. The model also suggests that the observed gamma rays are concentrated into an angle of order 1/η, implying a beamed or jet-like geometry. The energy sources in a cosmological context could be either stellar collapse or compact binary mergers.