# ASKAP Detection of Periodic and Elliptically Polarized Radio Pulses from UV Ceti

## TL;DR

This study reports ASKAP observations of UV Ceti revealing periodic, polarized radio pulses caused by electron cyclotron maser instability, indicating auroral activity in active M-dwarfs and demonstrating ASKAP's effectiveness in detecting such phenomena.

## Contribution

First detection of periodic, elliptically polarized radio pulses from UV Ceti using ASKAP, linking stellar auroral activity to magnetospheric processes.

## Key findings

- Detection of periodic, polarized radio pulses from UV Ceti.
- Evidence of electron cyclotron maser instability in stellar emission.
- Confirmation of auroral activity in active M-dwarfs.

## Abstract

Active M-dwarfs are known to produce bursty radio emission, and multi-wavelength studies have shown that Solar-like magnetic activity occurs in these stars. However, coherent bursts from active M-dwarfs have often been difficult to interpret in the Solar activity paradigm. We present Australian Square Array Pathfinder (ASKAP) observations of UV Ceti at a central frequency of 888 MHz. We detect several periodic, coherent pulses occurring over a timescale consistent with the rotational period of UV Ceti. The properties of the pulsed emission show that they originate from the electron cyclotron maser instability, in a cavity $\sim7$ orders of magnitude less dense than the mean coronal density at the estimated source altitude. These results confirm that auroral activity can occur in active M-dwarfs, suggesting that these stars mark the beginning of the transition from Solar-like to auroral magnetospheric behaviour. These results demonstrate the capabilities of ASKAP for detecting polarized, coherent bursts from active stars and other systems.