Ongoing Magnetospheric Accretion in the Multi-Ring Transitional Disk of HD 141569A

We present the results of long-term spectroscopic monitoring of the Herbig Ae star HD 141569A. The analysis is based on spectra obtained at the Shamakhy Astrophysical Observatory during 2017–2023 together with archival Ultraviolet and Visual Echelle Spectrograph (UVES) spectra acquired with the European Southern Observatory Very Large Telescope (ESO VLT) in 2007. Using synthetic model atmospheres, we investigated the emission structure of the hydrogen Balmer lines in the presence of strong photospheric absorption. The Hα and Hδ emission profiles exhibit double-peaked structures with central depressions, indicating that the emitting gas is in Keplerian rotation within the circumstellar disk. Peak velocities were used to estimate the emission radii of several hydrogen lines. We find an increase in the linear gas velocity together with a gradual decrease in the peak intensity ratio (IV/IR) from the outer to the inner disk regions. The Na i D, Ca ii K, and metallic absorption lines reveal outflowing gas with a velocity of approximately −13 ± 1.5 km s−1. Their narrow widths, significantly smaller than the stellar rotational velocity, suggest formation within an optically thick circumstellar wind. The hydrogen, Na i, and He i λ5876 lines show spectroscopic signatures of ongoing accretion onto the star. Accretion rates derived from the Hγ and Hδ lines yield the most reliable lower limit to the mass accretion rate, Ṁacc≈ (0.85--0.93)× 10⁻⁸\, M_ \, yr⁻¹. These findings demonstrate that magnetospheric accretion onto HD 141569A remains active despite its highly evolved multi-ring transitional disk.