In this work, we aim at understanding the dynamics of the magnetic star-disk interaction process in young stellar objects. We present the case of the young star, V2129 Oph, a well-known T Tauri star with spectral type K5, located in the rho Oph star formation region. We performed the time series analysis of this star using high-resolution spectroscopic data at optical wavelengths, from CFHT/ESPaDOnS and ESO/HARPS, and at infrared wavelengths, from CFHT/SPIRou. This dataset reveals a possible accretion variation over a time scale of a decade when compared to a previous observational campaign. We analyzed the variability of different circumstellar lines, such as Halpha and Hbeta, in the optical, and HeI (10830Å) and Pabeta, in the infrared. We measured the periodicity and the correlation matrices of these lines. We show that the optical and the infrared line profile variations are consistent with a magnetospheric accretion scenario with a period of ~6days, smaller than the stellar rotation period 6.53days. Additionally, the optical lines present strong indications of a structure located beyond the co-rotation radius, which is modulated at a period of about 8.5days. We investigate whether a wind component, twisted or multiple accretion funnel flows, or an external disturbance in the inner disk could explain this structure. This work shows how much variable is the dynamics of this system on a time scale of a few years.