Phenomenology and periodicity of radio emission from the stellar system AU Microscopii

Article


Bloot, S., Callingham, J. R., Vedantham, H. K., Kavanagh, R. D,, Pope, B. J. S., Climent, J. B., Guirado, J. C., Peña-Moñino, L. and Pérez-Torres, M.. 2024. "Phenomenology and periodicity of radio emission from the stellar system AU Microscopii." Astronomy and Astrophysics: a European journal. 682. https://doi.org/10.1051/0004-6361/202348065
Article Title

Phenomenology and periodicity of radio emission from the stellar system AU Microscopii

ERA Journal ID1050
Article CategoryArticle
AuthorsBloot, S., Callingham, J. R., Vedantham, H. K., Kavanagh, R. D,, Pope, B. J. S., Climent, J. B., Guirado, J. C., Peña-Moñino, L. and Pérez-Torres, M.
Journal TitleAstronomy and Astrophysics: a European journal
Journal Citation682
Article NumberA170
Number of Pages16
Year2024
PublisherEDP Sciences
Place of PublicationFrance
ISSN0004-6361
1432-0746
Digital Object Identifier (DOI)https://doi.org/10.1051/0004-6361/202348065
Web Address (URL)https://www.aanda.org/articles/aa/full_html/2024/02/aa48065-23/aa48065-23.html
AbstractStellar radio emission can measure a star’s magnetic field strength and structure, plasma density, and dynamics, and the stellar wind pressure impinging on exoplanet atmospheres. However, properly interpreting the radio data often requires temporal baselines that cover the rotation of the stars, orbits of their planets, and any longer-term stellar activity cycles. Here we present our monitoring campaign on the young, active M dwarf AU Microscopii with the Australia Telescope Compact Array between 1.1 and 3.1 GHz. With over 250 h of observations, these data represent the longest radio monitoring campaign on a single main-sequence star to date. We find that AU Mic produces a wide variety of radio emission, for which we introduce a phenomenological classification scheme predicated on the polarisation fraction and time-frequency structure of the emission. Such a classification scheme is applicable to radio emission from other radio-bright stars. The six types of radio emission detected on AU Mic can be broadly categorised into five distinct types of bursts, and broadband quiescent emission. We find that the radio bursts are highly circularly polarised and periodic with the rotation period of the star, implying that the emission is beamed. It is therefore most likely produced by the electron cyclotron maser instability. We present a model to show that the observed pattern of emission can be explained by emission from auroral rings on the magnetic poles. The total intensity of the broadband emission is stochastic, but we show that its circular polarisation fraction is also periodic with the rotation of the star. Such a periodicity in the polarised fraction of emission has not been observed on an M dwarf before. We present a qualitative model to describe the periodicity in the polarisation fraction of the broadband emission, using low-harmonic gyromagnetic emission. Using a simple qualitative model, we infer a magnetic obliquity of at least 20° from the observed variation in polarisation fraction. Finally, we show that the radio emission might be evolving on long timescales, hinting at a potential stellar magnetic activity cycle.
Keywordsradio continuum: stars
Contains Sensitive ContentDoes not contain sensitive content
ANZSRC Field of Research 20205101. Astronomical sciences
Byline AffiliationsNetherlands Institute for Radio Astronomy, Netherlands
University of Groningen, Netherlands
Leiden University, Netherlands
Centre for Astrophysics
University of Queensland
Polytechnic University of Valencia, Spain
Valencian International University, Spain
Institute of Astrophysics of Andalusia, Spain
University of Zaragoza, Spain
European University Cyprus, Cyprus
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