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Classical T Tauri stars are young low-mass systems still accreting materialfrom their disks. These systems are dynamic on timescales of hours to years.The observed variability can help us infer the physical processes that occur inthe circumstellar environment. We aim at understanding the dynamics of themagnetic interaction between the star and the inner accretion disk in youngstellar objects. We present the case of the young stellar system V2129 Oph,which is a well-known T Tauri star. We performed a time series analysis of thisstar using high-resolution spectroscopic data at optical and infraredwavelengths from CFHT/ESPaDOnS, ESO/HARPS and CFHT/SPIRou. The new data setsallowed us to characterize the accretion-ejection structure in this system andto investigate its evolution over a timescale of a decade via comparisons toprevious observational data. We measure radial velocity variations and recovera stellar rotation period of 6.53d. However, we do not recover the stellarrotation period in the variability of various circumstellar lines, such asH$\alpha$ and H$\beta$ in the optical or HeI 1083nm and Pa$\beta$ in theinfrared. Instead, we show that the optical and infrared line profilevariations are consistent with a magnetospheric accretion scenario that showsvariability with a period of about 6.0d, shorter than the stellar rotationperiod. Additionally, we find a period of 8.5d in H$\alpha$ and H$\beta$ lines,probably due to a structure located beyond the corotation radius, at a distanceof 0.09au. We investigate whether this could be accounted for by a windcomponent, twisted or multiple accretion funnel flows, or an externaldisturbance in the inner disk. We conclude that the dynamics of theaccretion-ejection process can vary significantly on a timescale of just a fewyears, presumably reflecting the evolving magnetic field topology at thestellar surface.

Star-disk interaction in the T Tauri star V2129 Oph: An evolving accretion-ejection structure