  Classical T Tauri stars are low-mass objects, which are still accreting
material from the surrounding circumstellar disk. The accretion process is
essential in the formation of Sun-like stars and in setting the properties of
the disk at the time when planet formation occurs. We constructed a complex
dataset in order to examine the accretion process of VW Cha, a classical T
Tauri multiple system with the aim of studying the physical origin of the
photometric and spectroscopic variability of the system. The TESS Space
Telescope observed VW Cha between 2019 April 22 and June 19, and we
complemented these data with contemporaneous ground-based $I_CJHK$ band
photometric measurements. In addition, we obtained high-resolution optical
spectra with the VLT/ESPRESSO and the 2.2\,m/FEROS instruments. Analyzing these
data, we found that the TESS light curve shows photometric variations on
timescales from minutes to weeks with a peak-to-peak amplitude of $\sim$0.8
mag. The near-infrared light curves follow the shape of the optical
measurements, however, the peak-to-peak amplitudes are slightly increasing
towards the longer wavelengths. We took spectra in both fainter and brighter
photometric states of the system, allowing us to examine the origin of a
photometric brightening event. Our results show that this brightening event can
be explained by increased accretion. In addition, our spectroscopic data also
suggest that the primary component of VW Cha is a spectroscopic binary, as it
was proposed in earlier works.
