The Role of Binary Configuration in Shaping Nova Evolution via Wind Accretion in Symbiotic Systems (2511.14596v1)

Abstract: We investigate the impact of the Bondi--Hoyle--Lyttleton (BHL) accretion mechanism on the evolution of nova eruptions in symbiotic systems by systematically varying three key input parameters: the initial donor (asymptotic giant branch; AGB) mass, the initial white dwarf (WD) mass, and the initial binary separation ($a$). We explore models with AGB masses in the range $1.5$--$3.5\,{\rm M_{\odot}}$, WD masses in the range $0.7$--$1.25\,{\rm M_{\odot}}$, and separations in the range $1$--$8\,{\rm kR_{\odot}}$. We find that all models exhibit a significant long-term orbital increase. This trend is primarily driven by the fact that approximately $99\%$ of the AGB mass is lost from the system, either directly via a wind that is not accreted by the WD, or accreted onto the WD and subsequently ejected during nova eruptions. As a result, the secular orbital response to mass loss or mass transfer dominates over angular-momentum-loss sinks that could otherwise shrink the orbit, producing a consistent orbital widening. Consequently, all WD masses gradually decrease with time. More massive WDs achieve higher mass-transfer efficiencies and accretion rates, leading to slightly higher mass-retention efficiencies per nova. However, because higher accretion rates also produce more frequent eruptions, the total WD mass lost over the AGB lifetime is larger in these systems. We conclude that symbiotic systems transferring mass via the BHL mechanism are unlikely to be viable progenitors of Type Ia supernovae.