SIMBAD references

We derive stringent constraints on the persistent source associated with FRB 121102: size 0.3 R_17.5 =(R/10^17.5 cm) 3, age 10^2.5 year, energy E~10⁴⁹(ε_e/0.2GeV)³ erg, characteristic electron energy 0.1 ε_e/1 GeV 0.5; the radiating plasma is confined by a cold plasma of mass M_c 10^–1.5R_17.5⁴ M_☉; these properties are inconsistent with typical "magnetar wind nebulae" model predictions. The fact that ε_e∼m_pc² suggests that the hot plasma was created by the ejection of a mildly relativistic, M~E/c²~10^–5 M_☉ shell, which propagated into an extended ambient medium or collided with a pre-ejected shell. Independent of the persistent source model, we suggest a physical mechanism for the generation of fast radio bursts (FRBs): the ejection from an underlying compact object, R_s=10⁶R_s,6 cm, of highly relativistic shells with energy E_s=10⁴¹E₄₁ erg and Lorentz factor γ_s=10³E₄₁^1/8R_s,6^–3/8, into a surrounding e - p plasma with density n∼10^–1 cm^–3 (consistent with that inferred for the persistent source). For E_s similar to observed FRB energies, plasma conditions appropriate for strong synchrotron maser emission at ν_coh.~0.5E₄₁^1/4R_s,6^–3/4 GHz are formed. A significant fraction of the deposited energy is converted to an FRB with duration R_s/c, accompanied by ∼10 MeV gamma-rays carrying less energy than the FRB. The inferred energy and mass associated with the source suggest some type of a "weak stellar explosion," where a neutron star is formed with relatively low mass and energy ejection. However, the current upper limit on R does not allow one to rule out M_c∼1 M_☉, or the ejection of a larger mass well before the ejection of the confining shell.