Mass-loss, composition and observational signatures of stellar winds from X-ray bursts

X-Ray bursts (XRBs) are powerful thermonuclear events on the surface of accreting neutron stars (NSs), which can synthesize intermediate-mass elements. Although the high surface gravity prevents an explosive ejection, a small fraction of the envelope may be ejected by radiation-driven winds. In our previous works, we have developed a non-relativistic radiative wind model and coupled it to an XRB hydrodynamic simulation. We now apply this technique to another model featuring consecutive bursts. We determine the mass-loss and chemical composition of the wind ejecta. Results show that, for a representative XRB, about $0.1\mathrm{\%}$ of the envelope mass is ejected per burst, at an average rate of $3.9\times {10}^{-12}{M}_{\odot }{\mathtt{\text{yr}}}^{-1}$. Between $66\mathrm{\%}$ and $76\mathrm{\%}$ of the ejecta composition is ${}^{60}$Ni, ${}^{64}$Zn, ${}^{68}$Ge, ${}^4$He and ${}^{58}$Ni. We also report on the evolution of observational quantities during the wind phase and simulate NICER observations that resemble those of 4U 1820-40.