Disambiguate the origin of asymmetric Fe I emission profiles

Determine whether the blueshifted excess and double-peaked asymmetric Fe I emission profiles in V1180 Cas arise from a hot disk wind or from other kinematic components in the inner accretion environment.

Background

The paper reports that optical-depth effects and self-absorption alone cannot explain the unequal, asymmetric Fe I emission profiles observed in V1180 Cas. Although the excess blue emission may indicate a hot disk wind, the available spectrum does not uniquely identify the responsible kinematic component. Resolving this issue would clarify the structure and dynamics of the inner accretion environment.

References

However, this interpretation remains tentative, as the present data do not allow us to uniquely distinguish between wind emission and other kinematic components within the inner accretion environment.

— Probing Accretion and Outflow in V1180 Cas through High-Resolution Optical Spectroscopy  (2610.01226 - Chand et al., 1 Oct 2026) in Section 4.1, subsection “Origin of the Permitted Line Emission”