Parkes observations for project P1119 semester 2022APRS_02

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Recently, low-frequency periodic radio pulses have been detected from the prototypical M-dwarf flare star, UV Ceti. This shows that the low-frequency emission from this star is driven by auroral activity, in stark contrast to the solar-like coronal activity exhibited at microwave–X-ray wavelengths. However, the driver of this auroral activity is unclear. Possible drivers of this aurora include breakdown of co-rotation with a magnetospheric plasma disk, or the sub-Alfv\\'enic interaction of the star with a companion planet. Expected signatures of the latter mechanism include small deviations of the radio pulse period from the stellar rotation period, or a modulation of the pulsed radio emission at the planetary orbital period. To detect these signatures, we require long-term, wide-band monitoring of the radio pulses. In this proposal, we seek to accurately measure the pulse rotation period of UV Ceti by measuring the pulse arrival times over four epochs separated by timescales of days--weeks. This will form an important part of the groundwork for detecting signatures of the auroral engine in future long-term monitoring. If successful, this project will mark the first steps toward unveiling the signature of star-planet interaction in this benchmark M-dwarf. This will enable this type of emission to be used as a future probe of exoplanetary systems.