2026-07-072026-07-07http://salesiana.dossiersoluciones.com/handle/123456789/159879Mode identification is crucial for an asteroseismological study of any significance. Contrarily to spectroscopic techniques, methods such as period-fitting and multi-colour photometry do not provide a full reconstruction of non-radial pulsations. We present a new method of spectroscopic mode identification and test it on time-series of synthetic spectra appropriate for pulsating subdwarf-B stars. We then apply it to the newly discovered slowly pulsating subdwarf-B star HD 4539.Presented at the "Third Meeting on Hot Subdwarf Stars and Related Objects"Astrophysicstext