Abstract We report photometric observations in Johnson B and V bands of the short term variability (flickering) of Mira (omicron Ceti). The observations were performed during 7 nights in the period August - October 2025, in the course of the last minimum of the Mira pulsations. The observed peak-to-peak amplitude of the flickering is 0.11-0.28 mag in B band. For the flickering source we find luminosity in the range 0.10 − 0.46 L⊙. Using the amplitude-flux relation, we estimate an average luminosity of the accretion disc Ld = 0.91 ± 0.28 L⊙. Assuming that the white dwarf accretes material through Wind Roche Lobe Overflow (WRLOF), we find that Mira B is a low mass white dwarf with Mwd = 0.24 ± 0.04 M⊙ accreting at a rate 6.8 × 10−9 M⊙ yr−1. This value of the mass is in the range of the extremely low mass white dwarfs. The data will be available on Zenodo.
Zamanov et al. (Mon,) studied this question.
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