English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The search for exoplanetary radio emission has resulted in zero conclusivedetections to date. Various explanations for this have been proposed, from theobserved frequency range, telescope sensitivity, to beaming of the emission. Ina recent paper, we illustrated that exoplanets can orbit through the radiophotosphere of the wind of the host star, a region that is optically thick at aspecific frequency, for a large fraction of their orbits. As a result, radioemission originating from the planet could be absorbed or `eclipsed' by thewind of the host star. Here we investigate how the properties of the stellarwind and orbital parameters affect the fraction of the orbit where the planetis eclipsed by the stellar wind. We show that planets orbiting stars with lowdensity winds are more favourable for detection in the radio. In terms of theorbital parameters, emission from transiting planets can escape the stellarwind easiest. We apply our model to the $\tau$~Boo planetary system, and showthat observing the fraction of the planet's orbit where it is eclipsed by thewind of the host star could be used to constrain the properties of the stellarwind. However, our model developed would need to be used in conjunction with aseparate method to disentangle the mass-loss rate and temperature of thestellar wind.

Radio eclipses of exoplanets by the winds of their host stars