Separate accretion-flow and outflow contributions to He I emission

Determine whether the broad, slightly blueshifted He I λ5876 emission component in V1180 Cas is produced by magnetospheric accretion flows, outflowing gas, or both.

Background

The He I λ5876 profile is decomposed into a narrow component associated with a post-shock accretion region and a broad component that may trace either magnetospheric accretion flows or an inner disk wind. The line profile alone cannot distinguish these physical origins, leaving the interpretation of the broad component unresolved.

References

Such broad, slightly blueshifted He I emission profiles have been associated with both magnetospheric accretion flows and outflowing gas in the inner star--disk environment; however, the present line profile alone does not allow us to uniquely distinguish between these contributions.

— 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”