Pulsational variability in the TESS light curve of HD46190

The new photometric data on the δ Scuti star HD46190 (TIC150394126) obtained recently with the Transiting Exoplanet Survey Satellite (TESS) are analysed to search for stellar pulsations. From the best fit of Balmer line profiles with a synthetic spectrum we have estimated its Teff = 8640 ∓ 100 K, log g = 4.0 ∓ 0.1, metallicity [M/H] = -0.7 ∓ 0.1, and substantial rotational velocity v sin(i) = 235 ∓ 2 km/s. Our analysis of the light curve accumulated over one year shows that HD46190 exhibits stellar pulsations with significant amplitudes (SNR > 4) in the spectral domain from 0.15 to 112 d^-1. For the signals detected in the domain from 35 to 70 d^-1 the best fitting model with 2 M⊙ and age around 5.44x10⁸ years corresponds to the large frequency separation Δν= 4.75 d^-1 and the core hydrogen fraction fov = 0.33. For two signals at 49.088 d^-1 and 58.583 d^-1 with the highest amplitudes we have found a long term variability of their amplitudes with time, which is most probably caused by beating of two or more nearby frequencies.